adsabs/AstroCLIMB huggingface dataset:
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Results of the juliet joint fit to the Unistellar photometry. Top: photometric data from the 13 eVscopes phase-folded to the period of TOI-4465 b. The gray band is the best-fit juliet transit model with 1σ uncertainty. The binned data (red points) with error bars are shown for clarity. The data are binned in 20-minute intervals. Bottom: residuals after the data have been subtracted from the best-fit model.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: NIR AO imaging and sensitivity curves for the Palomar Observations. Insets: image of the central portion of the image.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. VI. Confirmation of a Long-period Giant Planet Discovered with a Single TESS Transit
Authors: Zahra Essack, Diana Dragomir, Paul A. Dalba, Matthew P. Battley, David R. Ciardi, Karen A. Collins, Steve B. Howell, Matias I. Jones, Stephen R. Kane, Eric E. Mamajek, Christopher R. Mann, Ismael Mireles, Dominic Oddo, Lauren A. Sgro, Keivan G. Stassun, Solene Ulmer-Moll, Cristilyn N. Watkins, Samuel W. Yee, Carl Ziegler, Allyson Bieryla, Ioannis Apergis, Khalid Barkaoui, Rafael Brahm, Edward M. Bryant, Thomas M. Esposito, Pedro Figueira, Benjamin J. Fulton, Samuel Gill, Andrew W. Howard, Howard Isaacson, Alicia Kendall, Nicholas Law, Michael B. Lund, Andrew W. Mann, Rachel A. Matson, Felipe Murgas, Enric Palle, Samuel N. Quinn, Alexandre Revol, Suman Saha, Richard P. Schwarz, Ramotholo Sefako, Avi Shporer, Ivan A. Strakhov, Steven Villanueva, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Pau Bosch-Cabot, Kevin I. Collins, Raquel Forés-Toribio, Fabian Rodriguez Frustagia, Eric Girardin, Ian J. Helm, Pablo Lewin, Jose A. Muñoz, Patrick Newman, Peter Plavchan, Gregor Srdoc, Chris Stockdale, Anaël Wünsche, Mario Billiani, Martin Davy, Alex Douvas, Keiichi Fukui, Bruno Guillet, Cory Ostrem, Michael Rushton, Angsar Schmidt, Andrea Finardi, Patrice Girard, Tateki Goto, Julien S. de Lambilly, Liouba Leroux, Fabrice Mortecrette, John W. Pickering, Michael Primm, Marc Ribot, Ethan Teng, Aad Verveen, Stefan Will, Mark Ziegler
Figure caption: Posterior distribution for the joint (photometric + RV) model parameters derived with juliet.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Hα image of the region surrounding RS Oph, which is indicated by diagonal red ticks. The proper motion of RS Oph (with a Gaia-measured amplitude of 6.11 mas yr−1) is shown as a white arrow, whose length corresponds to the motion of RS Oph in the past 50 kyr. The positions of two inner and one outer SALT RSS slits, described in Section 2, are shown as yellow, magenta, and cyan lines, respectively. The image has been smoothed via a Gaussian kernel (σ = 3 pixels) and is displayed with linear scaling. The direction of proper motion of RS Oph is approximately perpendicular to the linear feature marked by yellow brackets in Figure 1, suggesting that this feature might be material snow-plowed by RS Oph.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Difference images (narrowband minus luminance) of the area surrounding RS Oph. Images have been 8x8 block-summed and are displayed with linear scaling. RS Oph is marked with red ticks. The NSR is now apparent in the Hα, [N II], and [S II] filters.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Condor narrowband images of the area surrounding RS Oph in He II, [O III], He I, H α, [N II], and [S II] filters. RS Oph is marked with red ticks. Images have been 8 × 8 block-summed and are displayed with linear scaling. The RS Oph NSR is immediately apparent only in the Hα image as a nebulosity filling much of the field of view and bounded by a nearly 1 degree long linear feature running northeast to southwest at the southern edge of the image.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Top: same as Figure 7, but the spectrum is sky-subtracted. Bottom: a close-up of the sky-subtracted region around Hα in Figure 8(a). The black, gray, and purple pixels are, respectively, at least 200, 20, and 2 counts above background.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Red, green, and blue image of RS Oph (position indicated with red ticks) and its surrounding emission. Each of the three channels is a block-summed difference image (see Figure 3). Blue corresponds to Hα–luminance; green corresponds to [N II]–luminance; and red corresponds to [S II]–luminance. The intensity scaling of each channel has been adjusted individually to highlight the emission features.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Hα–luminance difference image of RS Oph NSR (same as in Figure 2) with an overlaid sketch of the most prominent Hα emission. Two lobes of nebulosity are seen.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: SALT spectrum of the inner RS Oph shell taken on 2023 August 10 with the magenta-colored slit of Figure 6. All unidentified (vertical) lines are due to the night sky. Unidentified horizontal lines are field stars that were aligned with the slit during the observations.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Same as Figure 4, but after the “star-cleaning” algorithm STARNET2 is applied. The location of RS Oph is indicated with red ticks.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Top: measured radial velocity of the Hα line along the extent of the northern (cyan-colored) slit. Data were binned into 10″ wide bins to reduce noise. The velocity of each binned data point was determined relative to the nearest night-sky line at 655.35515 nm. The average velocity of Hα along the slit is -14.25 ± 0.74 km s−1. Middle: the FWHM of the Hα line along the northern slit is ∼ 15 km s−1, corresponding to 2.5 pixels on the detector. This demonstrates that the Hα line is unresolved. Bottom: the logarithms of the ratios of the [N II]658.4 /Hα and [S II]/Hα lines, both ∼−0.45, indicative of shock ionization. See the text.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: SALT spectrum of the outer RS shell shell, taken with the cyan-colored slit of Figure 6. All faint unidentified lines are due to the night sky.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Same as Figure 9, but the spectrum is sky-subtracted. All faint unidentified (vertical) lines are due to imperfectly subtracted night sky.
Paper: A 70 pc Diameter Nova Superremnant Surrounding the Recurrent Nova RS Ophiuchi
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Alexei Kniazev, Lee Townsend, David Zurek, Joanna Mikolajewska, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: The ratio of the forbidden [S II] line doublet 6716/6731 along the cyan-colored, “outer” shell SALT slit seen in Figure 6. The value of the line ratio is ∼1.41 ± 0.05, with individual points’ errors being ∼±0.10, consistent with an electron density of ≤∼50 electrons cm−3.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: An example of incorrect generation of the global view. For TIC 288323785, TESS acquired photometric data over a span of 3 yr (top panel). The transit mask (blue solid line), generated by using the period, epoch, and duration from the TCE, fits the data from sector 14 well (middle-left panel) but not the later ones (second and third middle panels). When flattening the light curves (black dots) dividing by the interpolating polynomial (red dashed line), transits from sectors 41 and 54 are not preserved. As a result, the light curve is not correctly phase-folded (bottom panel).
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: Data flow of our preparation pipeline. For each TCE, we downloaded the related FITS light-curve files from MAST. These light curves are concatenated in a single signal that is cleaned from not-a-numbers and outliers. The variability in the observed flux not related to the TCE’s transits is flattened in the detrending module. The resulting signal is folded over the TCE’s period. We finally binned and normalized the signal in order to produce a 201-length global view with median flux and transit depth set to 0 and −1, respectively.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: The white light phase curve of TOI-1685 b from 2.844 to 3.715 μm (NRS1, left column) and 3.823 to 5.172 μm (NRS2, right column) from JWST. Top: data from the Eureka! reduction (purple) and planet flux model fit to the data (gold). Bottom: residuals of the fit. Circles show binned data every 25 integrations to improve visualization.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: Variation of the main evaluation metrics (F1, precision, and recall) as the number of training epochs increases. These values have been computed on the test set of each data set. For sake of clarity, concerning TESS data we display the performance of DART-Vetter on the data set TESS that includes ExoFOP, Triple 9, and YU19.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: Mean values and error bars for F1-score, precision, and recall across all data sets. (Top panel, purple lines) Average scores and error bars computed for the specified evaluation metrics on the training sets. (Bottom panel, green lines) Corresponding values obtained on the test sets.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: As in Figure 1, but correcting for the instrument baseline trend of NRS1. Left is NRS1 and right is NRS2. The y-axis is zoomed in to see the planetary emission signal.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: Variation of the main evaluation metrics as the training and test data sets are split according to the different following ratios: 60–40, 70–30, 80–20, and 90–10. Each line shows the scores of F1 (left panel), precision (middle panel), and recall (right panel) for a given data set.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: Performance analysis of DART-Vetter on the Kepler Q1–Q17 Data Release 25 data set in the space defined by the parameters MES, Orbital Period, and Planet Radius. (Top row) Fractional values of precision (left) and recall (right) as a function of MES and Orbital Period. (Bottom row) Same values obtained as a function of MES and Planet Radius.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: An example of the output obtained by the horizontal reflection. From top left to bottom right we display six global views (blue lines) generated for six PCs KOIs from Kepler Q1 to Q17 DR25. For each global view, we provide its horizontally reflected version (orange lines). The horizontal reflection procedure is applied over all the data sets highly imbalanced toward the class of NPC.
Paper: DART-Vetter: A Deep Learning Tool for Automatic Triage of Exoplanet Candidates
Authors: Stefano Fiscale, Laura Inno, Alessandra Rotundi, Angelo Ciaramella, Alessio Ferone, Christian Magliano, Luca Cacciapuoti, Veselin Kostov, Elisa V. Quintana, Giovanni Covone, Maria Teresa Muscari Tomajoli, Vito Saggese, Luca Tonietti, Antonio Vanzanella, Vincenzo Della Corte
Figure caption: The architecture of the CNN model. The feature extraction branch is responsible for features extraction from the global view. The feature tensor produced by the last convolutional block is subjected to flattening. Then, classification is executed through utilization of a multilayer perceptron within the classification branch.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Results of the ICA for NRS2. We created 46 independent eigenvectors using the FastICA functionality in scikit-learn. We show the results for a single spectroscopic channel (λcen = 4.143 ± 0.017). Top: black is the reduced spectroscopic light curve. Purple is the light curve after it has been decorrelated against the four “best” eigenvectors, which are shown in the middle panel. The light curves are binned into 1 minute increments for ease of comparison. Bottom: results of the Lomb–Scargle periodogram on the four eigenvectors in the middle plot. Colors correspond to the appropriate eigenvector. As noted in the caption, through the ICA decorrelation, we decrease the OOT noise from 354 to 238 ppm. We defined the OOT regions as t = [(354.63, 354.85), (355.00, 355.20)] in units of BMJD 60000.5. We also note that even though there are little to no residuals of the transit and eclipses in the eigenvectors, the transit (orange-shaded region) and eclipse (yellow-shaded regions) depths change by 72, 4, and 135 ppm, respectively. The PCA eigenvectors behaved similarly. We conclude that while ICA and PCA can be used to remove similar systematics between light curves, it is best to proceed with caution when applying this technique to chromatic data sets.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Emission spectrum of TOI-1685 b using NIRSpec/G395H. Different data reductions follow the same color convention as Figure 4. Different symbols show different parts of the time series used in the fit as described in Section 3.2. Black circles represent the final emission spectrum from the prayer-bead analysis carried out in Section 3.3.3. The different data sets are offset slightly in wavelength to improve visualization.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Same as Figure 7, but for NRS1. While the ICA eigenvectors are able to successfully remove the linear trend seen in NRS1, nearly every eigenvector showed some residual signal around the transit. This made it challenging to remove the instrumental systematics through this technique without affecting the transit depth, as highlighted here. The eigenvectors for the PCA behaved similarly.
Paper: A Dark, Bare Rock for TOI-1685 b from a JWST NIRSpec G395H Phase Curve
Authors: Rafael Luque, Brandon Park Coy, Qiao Xue, Adina D. Feinstein, Eva-Maria Ahrer, Quentin Changeat, Michael Zhang, Sarah E. Moran, Jacob L. Bean, Edwin Kite, Megan Weiner Mansfield, Enric Pallé
Figure caption: Summary of transmission retrievals with TauREx. Left: best-fit spectra and transit observations (black data points) for TOI-1685 b. Right: probability density for the five runs including clouds. Our retrieval exploration rejects the clear primary atmosphere case. For the pure CO2 case, clouds can help reduce the 4.5 μm absorption feature, but this is not a statistically significant result (see Bayesian evidence in Table 4).