adsabs/AstroCLIMB huggingface dataset:
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: (a) K  s -band luminosity function of the cluster, reddened model control field, and control-field-subtracted cluster shown by orange, blue, and green histograms, respectively. The error bars represent the Poisson error. (b) K  s -band density plots of synthetic clusters of age 0.1, 0.5, 1.0, and 3.0 Myr, shown by solid curves. The dashed curves show the K  s -band density plots of the reddened control-field-subtracted cluster.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: (a) 13CO molecular gas distribution of G148.24+00.41. The green solid box here shows the inner cloud region zoomed-in in panel (b). (b) Herschel 250 μm image of the inner cloud region of size ∼35 pc × 25 pc (marked by a green solid box in panel (a)), along with small-scale filamentary structures adopted from Rawat et al. (2023). The green dashed box shows the hub region of size ∼2 pc × 2 pc, which is observed with TANSPEC. (c) NIR color-composite image (red: K  s  band; green: H band; and blue: J band) of FSR 655 as seen by TANSPEC. The location of the massive YSO (see text) is shown by a cross symbol.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption:  K  s  vs. H − K  s  diagram of the model population. The red dots show the background sources (d > 3.4 kpc) reddened by A V = 11 mag (average extinction toward the cluster). The colored curves show the main-sequence dwarfs locus reddened by A V = 0, 4, 11, and 22 mag. The blue arrow shows the reddening vector drawn from the 1 M ⊙ limit.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Density plots of photometric data of the cluster region in the J, H, and K  s  bands from the TANSPEC and 4.5 μm band from Spitzer. The dashed lines in all the panels show the completeness limiting magnitudes of 18.6 mag, 18 mag, 17.7 mag, and 14.9 mag in the J, H, K  s , and [4.5] μm bands, respectively.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Distribution of all the sources observed toward the cluster and the Besançon model generated sources, shown as a function of their (H − K  s ) colors. The blue and orange curves show the corresponding density plots of the cluster and model population, respectively.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Density plot of all the observed sources in the cluster as a function of their visual extinction (A V; see Section 3.2.1).
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: (a) Smoothened 2D density map of the sources, shown from the peak density up to the 10% level of stellar density. (b) Cumulative distribution of all the sources as a function of distance from the cluster center (marked by a cross in panel (a)). The dashed lines show the distances from the cluster center within which 50% and 90% of the sources are lying.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Color–color plots of 2MASS magnitudes vs. TANSPEC instrumental magnitudes in the J, H, and K  s  bands.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: (J − H, H − K  s ) CC diagram for the (a) cluster region and (b) modeled control-field region. The green curves are the intrinsic dwarf locus from Bessell & Brett (1988). The blue dots in panel (b) show the modeled field population. (c) (H − K  s , K−[4.5]) CC diagram for the cluster region. The brown curves are the intrinsic dwarf locus of late M-type dwarfs (Patten et al. 2006). In panels (a) and (c), the black dots show all the sources observed toward the cluster, and the red dots show the YSOs identified in the cluster, based on their NIR excess in the JHK  s  and HK  s [4.5] CC diagrams, respectively. In all the plots, the blue line represents the reddening vector drawn from the location of the M6 dwarf.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption:  H vs. H − K  s  color–magnitude diagram of sources in the cluster and control field. The black dots show all the sources observed in the cluster region. The green dots show the sample within A V = 4–22 mag. The blue dots show the foreground control-field sources, and the red dots show the background control-field sources, which are reddened to match the median visual extinction of the cluster region, i.e., A V = 11 mag. The MIST isochrones of 0.5 Myr (Choi et al. 2016) are reddened by A V = 4 and 22 mag and are shown in green curves. The blue arrows represent the reddening vectors, and the completeness limits of the data are marked by red dashed lines.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Visual extinction vs. age plot of different nearby clusters (d ≲ 4 kpc), given in Table 1. The black curve shows the best-fit exponential function (see text for details) with fitted parameters, a ≈ 26.30 ± 3.33 and b ≈ 1.26 ± 0.05. The red triangle shows the position of FSR 655. Here, the extinction values are corrected for foreground extinction, as found in the literature.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Cumulative initial mass function of the cluster. The red line shows the best-fit power-law mass function with index, α = 1.00 ± 0.15 for the mass range of 1–4 M ⊙.
Paper: Peering into the Heart of the Giant Molecular Cloud G148.24+00.41: A Deep Near-infrared View of the Newly Hatched Cluster FSR 655
Authors: Vineet Rawat, M. R. Samal, D. K. Ojha, Brajesh Kumar, Saurabh Sharma, J. Jose, Ram Sagar, R. K. Yadav
Figure caption: Spatial distribution of the sources visible in the 4.5 μm band, in the cluster direction within a 2′ radius from the cluster center. The location of the central massive YSO is marked by a yellow dot.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Top three panels: Phase-folded TESS FFI/HLSP and SPOC light curves of TOI-3261, with binned data in mauve and a best-fit batman transit model overlaid. Data taken at different cadences are displayed separately, as the observing cadences require different supersampling of the light curve to account for the change in transit shape. Bottom three panels: Phase-folded LCO light curves, with binned error bars included. These panels employ the same color scheme as the top three.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Lomb-Scargle periodograms derived from HARPS observations. The vertical dashed line denotes the period of TOI-3261b, while the horizontal lines represent computed 0.5%, 0.1%, and 0.01% False Alarm Probabilities. The topmost panel shows a peak at the planetary period, but the periodograms of the activity indicators (lower three panels) show no significant peaks near the 0.88 day mark. The peak at ∼8 days in the top panel is not astrophysical, as it disappears once the planet signal is removed.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Mass–radius distributions of ultrahot Neptunes compared to those of traditional USPs. The contour plot depicts the density in mass–radius space of the population of confirmed, published exoplanets listed in the Exoplanet Archive as of 2024 February 4. While the latter population is composed of pure rock, Neptune-sized USPs instead are expected to have a nonnegligible envelope atop a water-rich core. Overplotted are mass–radius relations for pure rock, pure water, and a combined rock/water core with various H2 mass fractions. The mass–radius relations based on planet composition are taken from Zeng et al. (2016).
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Phase-folded HARPS + ESPRESSO radial velocities of TOI-3261, with a best-fit RadVel model overlaid and residuals in the bottom panel. The pink crosses represent the HARPS data points, and the purple squares denote ESPRESSO data.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Multisector, raw TESS light curves of TOI-3261. Light curves from sectors 2, 6, and 13 are taken from FFIs with a 30 minute observing cadence. Sectors 27, 28, 29, and 36 show the 10 minute cadence FFI data. The Sector 63, 66, 67, 68, and 69 light curves depict SPOC 2 minute data.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: TOI-3261b in context with the published, confirmed exoplanet population as marked by the NASA Exoplanet Archive, as of 2024 February 4. The density map shows the distribution of confirmed exoplanets in radius-insolation space. The other Neptune-sized USPs are denoted in dark blue, with TOI-3261b represented in red. TOI-3261b sits squarely within the Hot Neptune Desert, shown by the dearth of Neptune-sized exoplanets at high irradiations.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Sensitivity curve of I-band delta-magnitude vs. on-sky separation, with a 4″ square image cutout inlaid. Centered on the star, the inset image shows the speckle autocorrelation function (ACF) of TOI-3261 observed with the High-Resolution Camera on the SOAR 4.1 m telescope. It has a pixel scale of 0.01575″ per pixel.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Stellar spectral energy distribution with an ATLAS9 model (T eff = 5000 K, [Fe/H] = 0 dex, log(g) = 4 dex) overlaid. Individual points represent photometric data from the Gaia DR2 Crossmatch Catalog. Horizontal errors denote the bandpass widths.
Paper: SOLES XII. The Aligned Orbit of TOI-2533 b, a Transiting Brown Dwarf Orbiting an F8-type Star
Authors: Thiago Ferreira dos Santos, Malena Rice, Xian-Yu Wang, Songhu Wang
Figure caption: Mass–radius diagram for the sample of known transiting brown dwarfs as of 2023 September (Carmichael 2023). The known transiting brown dwarfs to date with measured spin–orbit angles are indicated as black symbols. COND isochrones with ages 0.1, 0.5, 1, 5, and 10 Gyr, neglecting dust opacity in the radiative transfer equation, are indicated as dashed lines (top to bottom; Baraffe et al. 2003). For reference, the age of the TOI-2533 system (indicated as a blue dot) is estimated as ﹩{4.26}_{-1.74}^{+2.18}﹩ Gyr (Schmidt et al. 2023). Colors indicate the stellar effective temperature scaled by the Sun’s (T eff = 5772 K), and the shaded regions (left to right) show the boundaries for the deuterium-burning minimum mass (purple), lithium-burning minimum mass (blue), and hydrogen-burning minimum mass (pink).
Paper: SOLES XII. The Aligned Orbit of TOI-2533 b, a Transiting Brown Dwarf Orbiting an F8-type Star
Authors: Thiago Ferreira dos Santos, Malena Rice, Xian-Yu Wang, Songhu Wang
Figure caption: Distribution of the sky-projected spin–orbit angle ∣λ∣ as a function of the stellar effective temperature for brown dwarfs and exoplanets. TOI-2533 b, reported in this paper, is indicated in red. Background gray dots represent exoplanets presented in the TEPCat catalog (Southworth 2011) as of 2024 May, and black triangles indicate the four known transiting brown dwarfs with previously reported spin–orbit measurements (WASP-30 b, CoRoT-3 b, KELT-1 b, and HATS-70 b). The shaded blue area represents the approximate limits of the Kraft break, for which the precise location is a function of the stellar metallicity (Spalding & Winn 2022).
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Evolution of the radius of TOI-3261b as a function of varying initial envelope mass fractions, with a starting age of 10 Myr. These simulations assume a pure H/He envelope. The left, middle, and right panels show the planet’s radius evolution while experiencing low, intermediate, and high levels of stellar irradiation, respectively. The empty circle denotes the planet’s current radius and age, with the associated error bars for both parameters.
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Visualization of the radial location of fibers, shown on sky and on the NIRSPEC detector when observing with the KPIC FIU. One fiber is placed on the companion, one fiber is placed near the star, and the other fibers capture varying amount of stellar light. This NIRC2 image was not taken during the observing sequence but serves as an example of the dynamic range of the stellar halo though a coronagraph is not used during KPIC observations, so there is a slight difference. The right-hand image is a small portion of two echelle orders on the NIRSPEC detector, showing a portion of the fiber traces in those orders.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Evolutionary tracks of TOI-3261b’s mass (top panel) and radius (bottom panel), using models from Thorngren et al. (2023). These models assume an envelope enriched with metals. The planet’s mass loss is modeled at various initial and core masses. The point at which the track passes through the observed mass and radius is indicated by the purple squares.