adsabs/AstroCLIMB huggingface dataset:
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Color–color distributions of massive galaxies at 5 < z < 8.5 identified based on SED fitting w/wo MIRI photometry. Only galaxies with M⋆ > 2 × 1010M⊙ are shown, including sources with either M⋆,MIRI > 2 × 1010M⊙ (gray filled circles) or M⋆,noMIRI > 2 × 1010M⊙ (blue open circles). Right-pointing triangles indicate sources undetected in F150W (S/N < 2), whose F150W − F277W colors are derived from 3σ upper limits at F150W. The green shaded region shows the color-selection criterion used in I. Labbé et al. (2023) for selecting z ≳ 6 massive galaxies with V-shaped SEDs. The colored squares denote the evolution tracks for brown dwarfs (D. Langeroodi & J. Hjorth 2023; J. E. Greene et al. 2024) with a set of metallicities ([M/H] = −0.5 to +0.5), C/O ratios (from 0.5 to 1.5 times that of solar), and ages with cloudless atmospheres (M. S. Marley et al. 2021). The red filled circles denote LRDs. The number of M⋆ > 2 × 1010M⊙ galaxies drops significantly when MIRI is included: 31 with M⋆,MIRI > 1010.3M⊙ vs. 68 with M⋆,noMIRI > 1010.3M⊙. Most MIRI-confirmed massive galaxies lie outside the green shaded region and are not LRDs (LRD fraction: 4/31 with MIRI vs. 22/68 without MIRI).
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Example SED fits w/wo MIRI. Top: galaxies at z > 5 showing systematic M⋆ differences w/wo MIRI. Bottom: dusty galaxies at z ∼ 3 with significant M⋆ overestimation without MIRI. Orange circles and triangles show measured flux densities or 3σ upper limits (for nondetections) in different bands. Blue and black lines show the best-fit SED templates w/wo MIRI bands. The small blue and black points show model photometry. RGB false-color images (R:F444W, G:F277W, B:F150W) are shown in the lower-right corner of the corresponding SED plot. Adjacent to each SED plot, the panels in the right column show posteriors (probability density) for M⋆, dust attenuation, and mass-weighted (MW) age for each galaxy (w/wo MIRI). The dashed lines indicate 16%, 50%, and 84% intervals.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Redshift evolution of the observed ϵ and comparison to models. The data points show best-matched ϵ at different mass cuts and redshifts, based on M⋆ estimate for the primary sample (excluding LRDs) with MIRI photometry. The difference is that ϵ shown in the left panel is derived from the observed cumulative number densities of galaxies, while in the right panel they were obtained by integrating the intrinsic SMF (before convolution with a Gaussian kernel to account for the Eddington bias). The dotted lines show FFB models with ﹩{\epsilon }_{{\rm{\max }}}=0.2﹩ that best match our data (Z. Li et al. 2024). The dashed line shows CEERS results for M⋆ > 1010M⊙ galaxies based on NIRCam data only (K. Chworowsky et al. 2024).
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Differences in M⋆ estimates w/wo MIRI vs. redshift for galaxies at 2.5 < z < 8.5. Both panels show only MIRI/F770W-detected galaxies, with the left panel showing the high-mass subsample (M⋆,noMIRI > 1010M⊙) and the right panel showing the low-mass ones ((M⋆,noMIRI < 1010M⊙). The data points are color-coded by their local density. The y-axis shows the difference in M⋆ estimate w/wo MIRI, which is defined as ﹩{\rm{\Delta }}{M}_{\star }={\rm{log}}({M}_{\star ,{\rm{noMIRI}}}/{M}_{\star ,{\rm{MIRI}}})﹩. The red dashed line indicates the sliding median while the gray shaded region shows the 1σ (16%–84%) percentiles.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Comparison of photometric redshifts (zphot) derived with JWST/MIRI photometry against spectroscopic redshifts (zspec) for PRIMER galaxies. High-mass galaxies with M⋆ > 1010M⊙ are further denoted as red open circles, while LRDs are denoted as red crosses. Outlier rates (ORs; ∣Δz∣ > 3σNMAD × (1 + zspec)) for the whole sample and low- and high-mass subsamples are indicated in the top-left corner and are derived assuming the σNMAD value for the whole sample (0.017). σNMAD and ORs show no significant differences between high- and low-mass galaxies.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Stellar mass functions derived with (red circles) and without (blue triangles) MIRI at z ∼ 3–8. The filled red circles and blue triangles denote the data points with M⋆ derived w/wo MIRI data, respectively. The red and blue lines show best-fit Schechter functions (before convolution) for the data points w/wo MIRI data. The green dashed lines show best-fit Schechter functions including our primary sample and LRDs. The orange pentagrams show the stellar mass distribution of LRDs only, for which M⋆ are estimated using solely stellar templates.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Observed cumulative stellar mass densities compared to ΛCDM predictions for varying ϵ. The filled red circles denote the observed cumulative stellar mass densities based on our primary sample. The error bars indicate 1σ uncertainty that includes both Poisson errors and cosmic variance. The colored lines show predictions for four ϵ values given the assumed halo mass functions.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: Absolute B magnitude vs. effective temperature for a solar metallicity, 10 Myr MIST isochrone. The red dot marks the approximate location of Betelgeuse, and the blue box represents the possible boundaries for the stellar companion based on the estimated absolute B magnitude, the estimated uncertainty on that B magnitude, and where the absolute B magnitude boundaries intersect the isochrone. These values are in agreement with other works that predicted the presence of a companion (J. A. Goldberg et al. 2024; M. MacLeod et al. 2025).
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: Schematic diagram of the on-sky proper motion of Betelgeuse from 2020 (red) to 2024 (blue). [0, 0] is centered on the 2024 position of Betelgeuse, and the size of the circles represent the 40 mas angular diameter of Betelgeuse. The black dot shows the relative position of the detection to the 2024 position of Betelgeuse. This diagram shows that if the detection were a background star, it would have been detectable in our 2020 speckle observations.
Paper: The Probable Direct-imaging Detection of the Stellar Companion to Betelgeuse
Authors: Steve B. Howell, David R. Ciardi, Catherine A. Clark, Douglas A. Hope, Colin Littlefield, Elise Furlan
Figure caption: A highly stretched version of the 466 nm Betelgeuse image from UT 2024 December 9. The color scale is arbitrary and the image was used to determine the astrometric position of the companion relative to Betelgeuse. We find a separation of 52 mas and a position angle of 115°. The arrow points to the companion.
Paper: Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Authors: Tomoki Matsuoka, Keiichi Maeda, Ke-Jung Chen
Figure caption: Time evolution of velocity (upper left), density (upper right), ram pressure (lower left), and temperature (lower right) profiles in the SN–CSM interaction model possessing confined CSM with a mass-loss rate of ﹩\dot{M}=1{0}^{-4}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩. The SN ages are noted alongside each profile in units of days. Blue, red, and black lines indicate that the gas component is the SN ejecta, confined CSM, and tenuous wind CSM, respectively. The snapshots at the SN age of 1032 days are zoomed in and compared with Chevalier’s self-similar solutions with n = 5.5 (solid orange) and n = 12 (dashed cyan).
Paper: Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Authors: Tomoki Matsuoka, Keiichi Maeda, Ke-Jung Chen
Figure caption: Radio light curves constructed from our models. The black lines denote the temporal slope of optically thin emission in an adiabatic cooling phase. Note that the x-axis is the time since the shock breakout from the progenitor. Gray and red points are the observational data of SN 2001ig (S. D. Ryder et al. 2004) and SN 2003bg (A. M. Soderberg et al. 2006) at 4.8 GHz, respectively.
Paper: Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Authors: Tomoki Matsuoka, Keiichi Maeda, Ke-Jung Chen
Figure caption: Time evolution of the density structure in the model with ﹩\dot{M}=1{0}^{-4}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, but the x-axis is plotted by the mass coordinates (m) with the zero-point set to the contact discontinuity between the SN ejecta and the confined CSM. The color usage is the same as in Figure 1. m = MCSM in these mass coordinates corresponds to the contact discontinuity between two types of CSM, while the discontinuities seen in the confined CSM and tenuous wind are the reverse and forward shock, respectively.
Paper: Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Authors: Tomoki Matsuoka, Keiichi Maeda, Ke-Jung Chen
Figure caption: Top: time evolution of the density structure with the radius in the abscissa normalized by the forward shock radius at the given times. The color usage is the same as in Figure 1. Before t ≲ 10 days, the forward shock compresses the confined CSM component, and the heated confined CSM component is indicated by the red shaded region. After t ≳ 10 days, the newly formed forward shock heats up the tenuous wind, which is indicated by the shaded black region. The black dashed lines denote the reference density profiles of the ejecta with n = 12 and n = 5.5. Bottom: time evolution of the velocity structure with the radius normalized by the forward shock radius. Note that after t ≳ 10 days, the maximum velocity takes in the confined CSM component, indicating that it is a driving source for the expansion of the shocked shell.
Paper: Inferring a Dense Confined Circumstellar Medium around Supernova Progenitors via Long-term Hydrodynamical Evolution
Authors: Tomoki Matsuoka, Keiichi Maeda, Ke-Jung Chen
Figure caption: Time evolution of the forward shock velocity in our models. The dashed black lines denote the time dependence of ∝t−0.1 (corresponding to n = 12) and ∝t−0.28 (n = 5.5) for the reference.
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: The photometric and blackbody properties of SN 2025kg’s fast cooling phase compared to the early properties of the LFBOTs AT2018cow, ZTF18abvkwla, and AT2020xnd. Note that we have taken t0 = 58374.41 MJD for ZTF18abvkwla, i.e., the peak time in the g-band light curve.
Paper: The Kangaroo’s First Hop: The Early Fast Cooling Phase of EP250108a/SN 2025kg
Authors: Rob A. J. Eyles-Ferris, Peter G. Jonker, Andrew J. Levan, Daniele Bjørn Malesani, Nikhil Sarin, Christopher L. Fryer, Jillian C. Rastinejad, Eric Burns, Nial R. Tanvir, Paul T. O'Brien, Wen-fai Fong, Ilya Mandel, Benjamin P. Gompertz, Charles D. Kilpatrick, Steven Bloemen, Joe S. Bright, Francesco Carotenuto, Gregory Corcoran, Laura Cotter, Paul J. Groot, Luca Izzo, Tanmoy Laskar, Antonio Martin-Carrillo, Jesse Palmerio, Maria E. Ravasio, Jan van Roestel, Andrea Saccardi, Rhaana L. C. Starling, Aishwarya Linesh Thakur, Susanna D. Vergani, Paul M. Vreeswijk, Franz E. Bauer, Sergio Campana, Jennifer A. Chacón, Ashley A. Chrimes, Stefano Covino, Joyce N. D. van Dalen, Valerio D'Elia, Massimiliano De Pasquale, Nusrin Habeeb, Dieter H. Hartmann, Agnes P. C. van Hoof, Páll Jakobsson, Yashaswi Julakanti, Giorgos Leloudas, Daniel Mata Sánchez, Christopher J. Nixon, Daniëlle L. A. Pieterse, Giovanna Pugliese, Jonathan Quirola-Vásquez, Ben C. Rayson, Ruben Salvaterra, Ben Schneider, Manuel A. P. Torres, Tayyaba Zafar
Figure caption: A corner plot showing the parameter covariance in our fit to SN 2025kg’s fast cooling phase with a cooling, expanding blackbody.
Paper: On the Universality of the Split Monopole Black Hole Magnetosphere
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Spacetime plots of the normalized radial magnetic field on the event horizon for the four initial magnetic field configurations, shown as a function of time (horizontal axis) and cumulative surface coordinate ς (vertical axis). Colored regions mark opposite magnetic polarities, separated by a white interface indicating the current sheet where Br changes sign. Blue dashed lines show current sheet locations predicted by solving the ODE system (Equation (3)) of our model using initial conditions at t = 60rg/c, after pressure equilibrium is established.
Paper: On the Universality of the Split Monopole Black Hole Magnetosphere
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Time evolution of the normalized total absolute magnetic flux Φtot(t)/Φ0 through the event horizon showing simulation results (colored solid lines) and analytic model predictions (matching colored dashed lines). The vertical dotted line marks t = 60rg/c, the onset of pressure equilibrium that separates the two evolutionary phases. The top panel shows the flux evolution for the four simulated initial magnetic field configurations, and the bottom panel shows the evolution for five BH spins for an initial dipole configuration.
Paper: On the Universality of the Split Monopole Black Hole Magnetosphere
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Magnetic flux evolution of six 2D simulations of a nonspinning BH with an initial dipole magnetic field geometry, with increasingly higher resolutions showing numerical convergence. The left panel displays the time evolutions of the total instantaneous event horizon absolute magnetic field flux Φtot(t) normalized by the initial total event horizon absolute flux Φ0 = Φtot(t = 0). The vertical dotted line in both panels shows the time 60rg/c at which pressure equilibrium is established for all simulations, thereby separating the first pressure equilibration phase from the second pressure balance phase. The right panel displays the exponentially fitted flux decay timescales vs. the resolution shown by the number of computational cells in the polar direction.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Left panel: the best-fit eccentricity distributions of 2000 randomly generated eccentricity data sets of transiting long-period (10 days ≤ P ≲ 1000 days) giant planets (blue; Mc < 13.6 MJ), brown dwarfs (orange; 13.6 MJ ≤ Mc < 80 MJ), and low-mass stars (red; 80 MJ ≤ Mc ≤ 150 MJ), assuming truncated Gaussian distributions (see Section 4.2 for details). The best-fit shape parameters of the beta distribution (Equation (1)) are shown on the top right. Right panel: the distribution of best-fit shape parameter pairs of 2000 simulated data sets of giant planets (blue) and brown dwarfs (orange), consistent with each other within about 1σ. The vertical dashed lines show the best-fit parameters. The eccentricity distributions of transiting long-period brown dwarfs are similar to giant planets but different from low-mass stars.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Left panel: Keck/NIRES spectrum of TOI-5575 (black line) compared to the equivalent data for the M5 standard Gliese 866AB (magenta line; M. C. Cushing et al. 2005). Both spectra are normalized at 1.3 μm. Locations of major H2O and CO molecular absorption bands are labeled, as are regions of strong telluric absorption (gray boxes, masked in the spectrum of TOI-5575). The insets show close-ups of the 1.12–1.33 μm and 2.18–2.34 μm regions with primary atomic and molecular features labeled. Right panel: the SED of TOI-5575. The red crosses are the observed photometric measurements, where the horizontal bars represent the effective width of the passband. All blue dots represent the model fluxes from the best-fit PHOENIX atmosphere model (black solid lines). The Gaia spectrum is shown as a gray swathe in the inset panel.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Top panel: secondary component detection limits obtained using speckle imaging obtained with the speckle polarimeter on the SAI 2.5 m telescope. Bottom panel: Gemini high-resolution speckle imaging 5σ contrast limits as a function of angular separation. There are hints of a close companion in the reconstructed images, but these observations were taken at high air mass, and the orientation is consistent with the star being “smeared” along the parallactic angle, rather than being a close-in binary.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: The normalized TESS light curves of TOI-5575. The left, middle, and right panels are data from the Primary, First Extended, and Second Extended Missions. The light curve from the Primary Mission was extracted with a 3 × 3 pixel box aperture, while the light curves from the First and Second Extended Missions came from QLP and SPOC pipelines. The different transit depths seen in the three panels are likely due to the different aperture sizes, resulting in different light dilutions. The raw light curves are shown above in gray, while the detrended light curves are presented below in blue. The transits of TOI-5575 b are marked with red triangles. The transit event in Sectors 25 and 26 happened during the data gaps, so it does not show up.
Paper: A New Brown Dwarf Orbiting an M Star and an Investigation of the Eccentricity Distribution of Transiting Long-period Brown Dwarfs
Authors: Tianjun Gan, Charles Cadieux, Shigeru Ida, Sharon X. Wang, Shude Mao, Zitao Lin, Keivan G. Stassun, Adam J. Burgasser, Steve B. Howell, Catherine A. Clark, Ivan A. Strakhov, Paul Benni, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Luc Arnold, Étienne Artigau, David Charbonneau, Karen A. Collins, Neil J. Cook, Zoë L. de Beurs, Sarah J. Deveny, John P. Doty, René Doyon, Colin Littlefield, Tyler Pritchard, Gabrielle Ross, Avi Shporer, Christopher R. Theissen, Benjamin M. Tofflemire, Andrew Vanderburg, David Watanabe
Figure caption: Same as Figure 4 but using a/R* to select long-period systems. From top to bottom, they are results using a/R* ≥ 10, a/R* ≥ 15, and a/R* ≥ 20. The number of companions in each group is shown in the title of each panel.