adsabs/AstroCLIMB huggingface dataset:
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: 5σ contrast limits at J (bottom left), H (top left), and K (bottom right) from Gemini/NIRI and at ﹩{K}^{{\prime} }﹩ from Keck II/NIRC2 (top right). The combined images are shown in the insets of the panels, where Gliese 12 is at the star symbols. The maximum values of the image dynamic range were set to be 20 times higher than the noise levels at the edge areas. The locations corresponding to the identified possible source that was detected only in the J-band image are marked by arrow symbols and its contrast by a square symbol. Note that the source detection and contrast measurement were performed with the images after PSF subtractions.
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: (First–fourth rows) TESS PDCSAP light curves of Gliese 12 from Sectors 42, 43, 57, and 70, respectively. The locations of the predicted transits assuming P = 12.76 days are marked by vertical bars, where green and orange indicate odd- and even-numbered transits, respectively. The relative transit epochs are labeled beside the bars. The red solid lines shown in the second–fourth panels are the light curves predicted by the maximum-likelihood transit+GP model. (Bottom two rows) Same as above, but the data around each of the six transits covered by TESS are zoomed in. The transit epochs are shown on top of each panel. The gray dots and black circles are the unbinned and 30 minute binned data, respectively. The error bars of the binned data are shown, but they are smaller than the markers.
Paper: The Evolution of Stellar X-Ray Activity and Angular Momentum as Seen by eROSITA, TESS, and Gaia
Authors: Keivan G. Stassun, Marina Kounkel
Figure caption: (Top) Gyrochronology diagrams of the study sample represented by P rot versus stellar color. L  X , which correlates with stellar age, is represented by color. The usual “horseshoe shape” of relatively old (X-ray faint) and relatively slowly rotating stars defines the upper envelope (darker symbols), with relatively younger stars (X-ray bright) ranging down into the shorter rotation periods (lighter symbols). (Bottom) Relationship of L  X  with stellar ages determined independently by Kounkel et al. (2023). As expected, the younger stars at a given T eff generally exhibit stronger L  X . The eROSITA flux sensitivity limit at 200 pc, corresponding to the typical distance of stars in our study sample, is shown as a black line.
Paper: The Evolution of Stellar X-Ray Activity and Angular Momentum as Seen by eROSITA, TESS, and Gaia
Authors: Keivan G. Stassun, Marina Kounkel
Figure caption: Relationship of L  X  as a function of T eff across age for stars in 0.1 dex age bins. The red line corresponds to the running median of L  x  as a function of T eff at a given age. The best-fitted model for a given age is shown in the solid blue line. Other lines show the trend of the model with respect to age: in each panel, the dashed line is the model with ±0.3 dex difference from the given age, and the dotted line is ±0.6 dex difference. The scatter between the data and the model for a given age bin is shown in the corner. The symbols represent individual stars in the sample and are colored according to their angular momenta (L) relative to the median L in each age bin. It is evident that L contributes significantly to the apparent scatter in L  X .
Paper: The Evolution of Stellar X-Ray Activity and Angular Momentum as Seen by eROSITA, TESS, and Gaia
Authors: Keivan G. Stassun, Marina Kounkel
Figure caption: (Top) Relationship of L  X  with stellar angular momentum, L. As in Figure 1, L  X  varies with stellar age. However, it is also clearly apparent that, for stars of a given age, L  X  correlates strongly—and in a very simple manner—with L, and this L  X –L relationship is much simpler and tighter than the L  X –P rot relationship (bottom). The horizontal line in each panel is the same as in Figure 1.
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: TESS photometric apertures from Sectors 42, 43, 57, and 70 (gray outlines) with an archival image from the POSSII-F survey taken in 1988 (Reid et al. 1991), with Gaia DR2 source positions (Gaia Collaboration et al. 2018) shown as circles; the red circle denotes the Gaia position (at epoch J2015.5) of Gliese 12, which is offset from the position in the archival image due to the star’s proper motion, and the green circles show other sources.
Paper: The Evolution of Stellar X-Ray Activity and Angular Momentum as Seen by eROSITA, TESS, and Gaia
Authors: Keivan G. Stassun, Marina Kounkel
Figure caption: (Top) Representation of the full model fit (Equation (2)) for L  X  across the full range of L and stellar age. (Bottom) Same as top but for L = f(L  X , T eff) according to Equation (3).
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: GLS periodogram analysis of the IRD RV measurements, the spectra, and the light curves of Gliese 12. The solid, dashed, and dotted horizontal lines in each panel correspond to FAPs of 0.1%, 1%, and 5%, respectively. The vertical dashed and dotted lines correspond to P orb ≈ 12.76 days and P rot ≈ 85 days, respectively. (Left) GLS powers (green lines) for RV, window function, FWHM, dV, CRX, and dLW are plotted in the panels from top to bottom. (Right) GLS powers for the MEarth (top), ASAS-SN (middle), and SuperWASP (bottom) light curves. Orange lines indicate GLS powers for the light curves, and red lines indicate their window functions. P 1 (=108 days), P 2 (=83 days), P 3 (=85 days), and P 4 (=90 days) in the panels indicate the periods of four peaks in the GLS powers.
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: (Top left) Detrended (with the best-fit GP models), phase-folded, and 450 s binned transit light curves of Gliese 12 b. The data taken in the TESS, r, i, and z  s  bands are plotted from top to bottom. The gray lines represent the best-fit transit models. Each light curve is vertically shifted by an arbitrary value for display purposes. (Bottom left) Same as the top left panel, but residuals from the best-fit transit models are shown. (Top right) RV time series of Gliese 12 measured with IRD (red) and CARMENES (blue) along with the best-fit Keplerian model (light blue). The error bars represent 1σ uncertainties without including RV jitters. (Middle right) Same as the top right panel, but the data are phase-folded with the orbital period of Gliese 12 b. The error bars here represent 1σ uncertainties taking RV jitters into account. The darkest, second-darkest, and lightest light blue colors indicate the 1σ, 2σ, and 3σ confidence regions calculated from the joint analysis, respectively. (Bottom right) Same as the middle right panel, but the data are binned into 10 equally spaced bins.
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: TESS light curves (black dots) of Gliese 12 for the odd- (left) and even-numbered (right) transits. They were phase-folded for the P = 12.76 day ephemeris. Binned data points are shown as cyan-filled blue circles. The transit depths and 1σ uncertainties were determined from independent transit model fits to each light curve and are shown as horizontal red solid and dashed lines. The “Depth-sig” at the top of the plot is the statistical significance of the difference between the odd and even transit depths. The low significance (0.01σ) indicates there is no significant discrepancy in the measured depths between the two sets. The plots are reproduced from the DV report produced by the SPOC pipeline (Twicken et al. 2018) for Sectors 40–70 (the full report is available from MAST).
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: Individual transit light curves of Gliese 12 b obtained with MuSCAT2 and MuSCAT3. Columns from left to right show the data taken on the nights of UT 2023 July 22 (transit epoch = 51), August 16 (53), September 11 (55), and October 6 (57). The top, middle, and bottom rows are for the r, i, and z  s  bands, respectively. The top and bottom panels in each panel pair show the undetrended light curve and its residuals from the best-fit transit+GP model (colored line), respectively (see details in Section 4.2.2). For both panels, gray dots and black circles indicate unbinned and 15 minute binned data, respectively. Darker to lighter blue vertical bands indicate the 1σ, 2σ, and 3σ credible regions, respectively, of the midtransit times predicted from P and T c,0 derived from the analysis of the TESS light curves (Section 4.2.1).
Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: Predicted transmission spectra for Gliese 12 b, assuming an isothermal temperature–pressure profile, an Earth-like density, and several different cloud-free compositions: primordial H2 and He at 100× solar metallicity, Titan-like, water world, and Venus-like. For the Venus-like scenario, we also show a model including 0.1 bar fully opaque clouds. We show simulated data assuming the cloudy Venus scenario and six transits per JWST/NIRSpec grism: G140H (green squares), G235H (red circles), and G395H (blue diamonds).