adsabs/AstroCLIMB huggingface dataset:
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The binned TESS PDC light curves phase folded on the orbital period of HD 83443b (2.985 days) for Sector 9 (top left), Sector 35 (top right), Sector 36 (bottom left), and the concatenated light curve (bottom right). The red points show the binned photometry and their uncertainties show the standard deviation of the individual data points contained within each bin. The individual data points scatter beyond the shown flux limits and, thus, are not shown. The blue triangles indicate spacecraft thruster firing timings (i.e., momentum dumps). The black arrow indicates the expected time of transit at 0 phase and the gray curve shows an example of the expected phase modulations if the planet had 0.3 albedo. The observed modulations are inconsistent between TESS sectors and tend to align with momentum dump timings. Therefore, we conclude that we do not observe any evidence for transit events or phase modulations by HD 83443b.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Top down view of the HD 83443 system with both conservative and optimistic HZ regions shown in light green and dark green, respectively. The orbit of the outer planet is color coded with the planet-to-star flux ratio if the brightness is above 1 × 10−10, assuming near edge-on inclination. Part of the orbit with low flux ratios not color coded is due to the planet passing through the inner working angle of HabEx starshade. The inner b planet is not shown due to its proximity to the host star and the scale of the plot.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Eccentricity-semimajor axis distribution of exterior companions to Hot Jupiters. HD 83443c is shown as a star, and is the most distant, most eccentric such planet yet found. Each planet is color coded by its planetary mass value (or projected mass value if no radius measurement). The open circles represent known brown dwarf exterior companions. Planet data from NASA Exoplanet Archive, accessed 2021 November 15.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Model proper motions compared to the calibrated Hipparcos (point at 1991.25) and Gaia EDR3 proper motions (point at 2016) from the HGCA. The best-fit orbit is shown in black. A random sampling of other orbits from the MCMC chain are shown and are color coded by the mass of HD 83443c. Note that the fit to the long-baseline proper motion between Gaia and Hipparcos is not shown because it is an integral constraint.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Corner plot—starting orbital period: 10,000 days.
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: Corner plot—starting orbital period: 6000 days.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: HEB mass configurations, which produce eclipse depths in the g band (blue) and z band (red) consistent with the observed depths (indicated in the upper left corner of the first panel). The left panel corresponds to the lower limit of the impact parameter and the right for the median value. The colored solid line and dashed lines correspond to confidence regions that are consistent with the observed depths within 1 and 2σ, respectively. The vertical black line corresponds to the mass of the central star (i.e., TOI-1696). The fact that the red and blue regions do not overlap within 1σ taking into account impact parameter rules out the HEB false-positive scenario.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Initial H2/He atmospheric mass fraction of a TOI-1696 b-like planet that satisfies the radius of 3.09 ± 0.11 R ⊕ and T eq = 489 ± 13 K after photoevaporative mass loss for 8 Gyr under the standard XUV radiation field (L XUV) and 10L XUV. The gray region shows the H2/He atmospheric mass fraction that reproduces the observed radius of TOI-1696 b with a rocky core.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: SED of TOI-1696. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit NextGen atmosphere model (black).
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Joint and marginal posteriors for the key parameters from the transit+contamination modeling of the MuSCAT3 multicolor light curves. Contamination due to sources with significantly different effective temperatures than the host is ruled out.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Metallicity values derived from the IRD spectrum. The horizontal dashed line corresponds to the weighted average [M/H].
Paper: HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Authors: Adriana Errico, Robert A. Wittenmyer, Jonathan Horner, Zhexing Li, G. Mirek Brandt, Stephen R. Kane, Tara Fetherolf, Timothy R. Holt, Brad Carter, Jake T. Clark, R. P. Butler, C. G. Tinney, Sarah Ballard, Brendan P. Bowler, John Kielkopf, Huigen Liu, Peter P. Plavchan, Avi Shporer, Hui Zhang, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura
Figure caption: The dynamical stability of massless test particles in the HD 83443 system, for simulations considering a variety of orbital inclinations for the orbit of HD 83443c. The top left hand panel shows the case where the system begins in a fully coplanar state, with HD 83443c moving on an orbit that is in the same plane as the disk of test particles and the orbit of HD 83443b, as presented in Figure 2. The remaining panels feature simulations at lower resolution, following the evolution of 686,340 massless test particles. The central plot of the top row shows the outcome with HD 83443c moving on an orbit tilted by 5° to the disk and inner planet; top right has c on an orbit inclined by 15°; lower left has an inclination of 30°; lower center has an inclination of 45°, and lower right, 60°. As with Figure 2, the simulations spanned a period of 1 Myr. Again, since the simulations covered a period of 1 Myr, the regions in white are those where test particles have minimum lifetimes of 1 Myr. It is highly likely that, across much of that space, lifetimes would be far longer than the 1 Myr of our simulations. Moderate levels of mutual inclination between the orbits of the outer planet and the disk do little to alter the stability profile, but once the orbit of HD 83443c is inclined by 45° and 60°, it begins to whittle away at the outer edge of the stable area, rendering orbits in the region beyond ∼0.9 au (45°) and ∼0.5 au (60°) unstable on timescales of hundreds of thousands of years.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Gaia apparent G magnitude vs. Gaia BP–RP color for 451 candidate members of IC 2602 (left panel) and 350 candidate members of IC 2391 (right panel); the 14 candidate members without Gaia colors (4 in IC 2391 and 10 in IC 2602) are not plotted. For IC 2602, 331 are new (blue circles) while 120 are known (red triangles). For IC 2391, 198 are new (teal circles) while 152 are known (pink triangles). Objects brighter than G = 14 in the Gaia DR2 membership lists that are absent from ours are indicated by golden stars. The magenta line shows the brightness (G = 8) above which a more lenient parallax constraint is applied in identifying membership (see Section 2). Estimated spectral types are shown at their corresponding Gaia color (Pecaut & Mamajek 2013). We obtain optical spectra for all new candidate members brighter than G = 13 (see Section 3).
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Equivalent widths of lithium at 6708 Å are plotted against effective temperatures (see Section 3.3) for all observed stars in this study for IC 2602 (magenta squares; IC2602_n) and IC 2391 (cyan circles; IC2391_n). Upper limits are indicated with arrows. Here, we show that our lithium measurements for IC 2602 and IC 2391are consistent with those for other clusters of similar age (Gutiérrez Albarrán et al. 2020).
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Candidate photometric binaries are identified in IC 2602 by an iterative fit to the main sequence (down to G < 18). Stars retained in the fit are shown as yellow circles. For stars brighter than G = 14, any star more than 0.6 mag above the fit are considered candidate binaries (cyan circles). For stars fainter than G = 14 (blue circles), we do not identify binaries because of the broader main sequence.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Sky positions for IC 2602 and IC 2391 candidate cluster members identified using the prescription in Section 2. The R.A. and decl. ranges of search regions are shown and extend off the plot (brown for IC 2602 and purple for IC 2391). New and known IC 2391 candidate members are represented by red and blue points, respectively. New and known IC 2602 candidate members are represented by cyan and yellow points, respectively.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Metallicity is plotted against effective temperature for the 393 spectral standards (dwarf stars with 3 < log(g) < 5) used in the Empirical SpecMatch spectral library (red points). Previously known members and new candidate members observed in this study are colored green and blue, respectively. Stars are marked as squares if they are candidate double-lined spectroscopic binaries (see Section 4.2) and triangles if they are not.
Paper: Mapping out the Stellar Populations of IC 2602 and IC 2391
Authors: Azmain H. Nisak, Russel J. White, Alexandra Yep, Todd J. Henry, Leonardo Paredes, Hodari-Sadiki James, Wei-Chun Jao
Figure caption: Distribution of RVs for spectroscopically observed stars in IC 2602 (top panel) and IC 2391 (bottom panel) as a function of effective temperature. Candidate binary stars (blue squares) are identified by iterative fits to the mean RVs (dotted black lines) of the ensembles; yellow circles are not candidate binaries.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The relations between the magnitude of aberration coefficient c  jk  (waves in root mean square) of a particular order (j, k ≤ 3) and the averaged leaks that the aberration brings. The simulation is executed for the wavelength of 690 nm. The green solid curve indicates the case of (j, k) = (0, 0). The blue solid curves indicate the case in which one of j, k is zero and another is not zero. The red solid curves indicate the case in which neither of j, k is zero.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The leak-intensity map with respect to each order of the aberration on the last Lyot stop. The magnitude of the aberration coefficient c  jk  is assumed to 10−3 waves. The assumed observational wavelength is 690 nm.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The leak-intensity map with respect to each order of the aberration on the last focal plane. The magnitude of the aberration coefficient c  jk  is assumed to 10−3 waves. The assumed observational wavelength is 690 nm.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: Comparison of the results of numerical calculations of pupil leaks with different discretization: the result with the same mesh to discretize the focal plane as the one used in Section 3 (left) and the result with the mesh 16 times finer than the one used in Section 3 (right). The assumed observational wavelength is 700 nm.
Paper: A Coronagraph with a Sub-λ/D Inner Working Angle and a Moderate Spectral Bandwidth
Authors: Satoshi Itoh, Taro Matsuo
Figure caption: The Fourier conjugates of the base functions indicated in Figure 6. Since Fourier Transform preserves inner products of any two functions, these functions also have orthonormality.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: TOI-1696 b (blue point) in the context of known transiting planets (contours). TOI-1696 b appears to be within or close to the boundaries of the Neptunian desert (solid black lines) in the period–radius plane defined by Mazeh et al. (2016). The dashed lines refer to the boundaries’ uncertainty regions. Also shown are planets (orange points) orbiting M dwarfs (T eff < 3800 K) and the five planets (red points) most similar in this parameter space to TOI-1696 b: K2-25 b, K2-320 b, GJ 1214b, TOI-269 b, and TOI-2406b.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Transit model fit to the MuSCAT3 (M3) data from 2020 December 23, ordered column-wise per bandpass. The top row shows the raw data with the transit and systematics model, the middle row shows the systematics-corrected data with only the transit model, and the bottom row shows the residuals from the fit. The colors of the model correspond to the photometric bandpass of each data set; see also Figure 10.