adsabs/AstroCLIMB huggingface dataset:
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Caustic geometries of OGLE-2016-BLG-1850.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Caustic geometries of KMT-2016-BLG-0625 for the 2L1S models.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of KMT-2016-BLG-0625 with degenerate models.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Distribution of I diff (top), I srch (middle), and I tmpl (bottom) value for the 20,000 transients in the test data (see Equation (4)). The colors correspond to the quadrants of the confusion matrix to which the transient belongs according to the model prediction, with DIA-based predictions in the first and second columns and noDIA in the third and fourth. Blue shades correspond to correct predictions (TP and TN) and orange to FP and FN. Note that the y-axis values are different in each plot, and the FP and FN histograms contain far fewer observations. On the I tmpl, for the DIA-based model (left), the TP classification shows a preference for the diff images, and the distribution peaks at I diff ∼ 0.5. For TN, however, small I diff values are more common, with an significant fraction of observations in the 0 < I diff < 0.33 region. This behavior is complemented by a long I tmpl tail in the TN distribution (0.4 < I tmpl < 0.8). The FP and FN distributions are qualitatively similar to the TP and TN but noisier, as they contain fewer than 10% of the objects. Right: noDIA model. All four classes have qualitatively similar distributions in I tmpl and I srch. Classifications rely mostly on the tmpl in all cases (I tmpl > 0.5). The mathematical meaning of the plotted quantities is described in detail in Section 4.4. The figure is discussed in Section 5.1.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: =Transients (diff–srch–tmpl) and their respective saliency maps for DIA-based model TN predictions (correctly identified as bogus). A contour plot of light intensity from the original images is overplotted, delineating the bright sources. (a) I diff ∼ 0.4. (b) I diff ∼ 0.69. (C) I tmpl ∼ 0.42. In panel (c), the saliency for the tmpl portion of the image looks strikingly similar to the selection of pixels that is made in aperture photometry, with pixel values considered in the core of the source, ignored in a region immediately around the source, and again considered farther out to calculate the source’s background. This figure is further discussed in Appendix C.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (diff–srch–tmpl) and their respective saliency maps for DIA-based model FNs (real transients identified as bogus). We remind the reader that the labels are inherited from Goldstein et al. (2015) and cannot be verified. Some level of label inaccuracy is expected. The real transients in this data set are implanted SNe onto real DES images. However, in this collection, several transients display DIA inaccuracies (rows 1, 2, 4, and 6 show dipoles; see Section 2.1) that likely lead to the incorrect classification. Two very low signal-to-noise ratio detections are missed (rows 3 and 5) by our model. Important pixels are more commonly found in the diff portion of the image. In the srch saliency maps, we see again that the core of the central source is used in the classification, as well as the pixels that surround the source, but these two sets of important pixels are separated by a gap, again reminiscent of the typical aperture photometry technique (top two panels).
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (diff–srch–tmpl) and their respective saliency maps for DIA-based model TPs (correctly identified real astrophysical transients). The important pixels are generally found in the diff portion of the image for the DIA-based model, as discussed in Section 5, but there are exceptions. Here we show several cases of TP (real transient) classifications where the component of the image that was principally leveraged by the model was the diff (the leftmost third) but two cases where the noDIA relied principally on the srch and/or tmpl (bottom two panels).
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Same transients (srch–tmpl) as in Figure 15 and their respective saliency maps for noDIA model TNs (correctly identified as bogus). Important pixels are found at nearly all locations in the image, rather than in a small region around the center. The model needs to learn the properties of the image at large to enable a comparison of the tmpl and diff. This figure is further discussed in Appendix C.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Violin plot of pixel values inside the μ ± 3σ interval for the srch and temp images of the data shown in Figure 1 (before normalization). These values were scaled between zero and 1. The left and right curves correspond to the srch and temp distribution of values, respectively. The distribution of values corresponds to that shown in Figure 2 for srch and temp, and the green and purple colors correspond to Figure 2.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Same as Figure 5 (left) but for a DIA-based model that takes input data stacked in a depth axis, i.e., 5 × 151 × 3. Overall, the performance of the model is not significantly affected by the choice of input data, with an ∼1% decrease in the TN rate.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Violin plot of pixel values for the srch and temp images of the data shown in Figure 1 (after normalization). Values between the vertical lines in zero and 1 were mapped to the values in Figure 12. Negative values and above 1 correspond to the scaled values outside the 3σ clip.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (srch–tmpl) and their respective saliency maps for the noDIA model TPs (correctly identified real astrophysical transients). Important pixels are found everywhere in the image, as the CNN learns how to compare the diff and tmpl by taking a synoptic look at the properties of each image component.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Posterior distributions for the chemical equilibrium retrieval which included an offset in the HST WFC3 G141 data. The retrieval converges to a solution which has a significant offset. However, the Bayesian evidence for this retrieval is significantly less than that of the same retrieval minus an offset parameter. The difference in the Bayesian evidence suggests an offset between the data sets is rejected at the 3.4σ level, the same degree to which the free chemistry retrievals prefer a lack of offset.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Posterior distributions for the free chemistry retrieval which included an offset in the HST WFC3 G141 data. The retrieval converges to a solution which has a slight offset, but the “no offset” solution is well within the 1σ uncertainties. Furthermore, the Bayesian evidence for this retrieval is significantly less than that of the same retrieval minus an offset parameter. The difference in the Bayesian evidence suggests an offset between the data sets is rejected at the 3.7σ level.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Posterior distributions for our preferred chemical equilibrium retrieval which included a nonisothermal temperature profile. We note that this retrieval was not preferred over the free chemistry model given in Figure 19, with the Bayesian evidence preferring the latter to 2.4σ. Additionally, while the nonisothermal temperature profile led to a preferable fit, it did not led to a well-constrained temperature–pressure profile.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Posterior distributions for our preferred free chemistry retrieval which included an isothermal temperature profile and two-layer abundances for H2O and CO2. We note that, for many parameters, the best-fit value is simply the mean of the prior.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Posterior distributions for our free chemistry retrieval which accounted for spots and faculae. The retrieval prefers a solution without an atmospheric detection for LTT 9779 b and instead favors a very large, and unlikely, faculae covering fraction.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: TESS light curves for TOI-199, for the seven sectors with transits. The short-cadence PDCSAP light curves are shown in blue, and the FFI light curves extracted with tesseract in orange. For Sectors 10 and 32 the transits could not be correctly recovered from the PDCSAP light curves.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: Follow-up photometry for TOI-199. Top row: light curves of ASTEP observations—an egress on 2021 March 31 (left), a full transit on 2021 July 13 (center), and a full transit on 2022 September 06 (right). Middle Row: light curves for PEST (left, egress on 2020 December 16), NEOSSat (center, full transit on 2021 March 31), and Hazelwood (right, egress on 2021 March 31) observations. Bottom row: light curves of LCO observations—a preingress flat curve on 2020 December 16 (left), two ingresses and egresses on 2022 February 08 (center), for which the points are color coded by filter and site, and a full transit on 2022 December 20 (right). In all panels, the dashed vertical line indicates the transit midpoint, and the dotted vertical lines the egress and ingress.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: LCO light curves (colored points) and fitted models (black lines) for the three transits observed with LCO. The data for transit 13 are colored by filter and site, as in Figure 2.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: TESS FFI light curves, extracted with tesseract (blue points), and fitted models (black lines) for the seven transits observed with TESS. The GP components of each model have been subtracted.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: O – C plot (difference between predicted and observed transit midpoint times) for the TESS, ASTEP, and LCO transits. The error bars are generally smaller than the marker size.
Paper: TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica
Authors: Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria Carleo, Karen A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou
Figure caption: ASTEP light curves (blue points) and fitted models (black lines) for the three transits observed with ASTEP.