adsabs/AstroCLIMB huggingface dataset:
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The SpeX spectrum (black) of each double-peaked H-band object is shown with its best-fit Sonora (blue dashed) and Phoenix (orange dashed) models. The first four digits of the R.A. coordinates of each object are given to the left. A reference spectrum made by averaging all L8–T1 objects from the sample is included at the bottom of the plot. The right panel shows just the H band of each object (black) along with its double-peaked fit (green) and trapezoidal fit (gray dashed).
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The objects with plateaued H-band peaks are marked in red at the tops of plots of the Sonora (left) and Phoenix (right) model best-fit temperature vs. IR spectral type (top) and 2MASS J − K color (bottom). These objects are all early T types and fall on the warmer end for their spectral types based on their Sonora temperatures. There is no apparent pattern according to their Phoenix temperatures. Objects in this family have fairly average colors for their spectral type.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots showing binary model fits to the six members of the double-peaked H-band family. The models are all Sonora models. The data and composite models are plotted in black and green, respectively, The orange and blue curves give the individual components that were summed together to generate the composite model. The parameters of the components are given above in Table 6.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots showing binary model fits to the five members of the plateaued H-band family. The models are all Sonora models. The data and composite models are plotted in black and green, respectively, The orange and blue curves give the individual components that were summed together to generate the composite model. The parameters of the components are given above in Table 4.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots of Sonora Elf Owl models (S. Mukherjee et al. 2024) with L–T-transition-type temperatures and varied C/O ratios. C/O ratio alone is not enough to explain the flat shapes of the plateaued H-band family members, since even the flattest models plotted here still show too much absorption around 1.6–1.65 μm.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The objects with double-peaked H bands are marked in red on top of plots of the Sonora (left) and Phoenix (right) model best-fit temperatures vs. IR spectral types (top) and 2MASS J − K color (bottom). All members of this family fall in the L–T transition. There is not a consistent trend in J − K color for this family.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Magnetic field orientation difference between the starlight polarization and polarized thermal dust emission from Planck Collaboration XII et al. (2020) as a function of distance in C5 (top left), C45 (top right), and C50 (bottom). Due to the π ambiguity, the angular difference range in C45 was shifted by 50° for visualization. For each region, the bottom panels show the weighted circular mean difference per distance bin using the NIR (the solid light-orange) and optical (the solid black) observations. The error bars are the weighted circular standard deviation on each distance bin. The vertical red dashed lines show the corrected distance of the polarizing clouds found with BISP-1. The right-side panels show the angular difference distributions with the circular means (the horizontal dashed lines). The two top panels show the projected Rayleigh statistic (PRS; Equation (6)) per distance bin along with the weighted error. The gray and orange shaded areas represent the values between the maximum and minimum PRS per distance bin (see explanation in Section 5.5).
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: GMM results with optical (left) and NIR (right) polarization in C5. Top row: Stokes parameters q(v, h) and u(v, h) as a function of distance. The different colors and symbols represent the groups identified by the GMM. The extinction density with units of 10−3 mag pc−1 from J. L. Vergely et al. (2022), at 10 pc (dark gray) and 50 pc (light-gray) resolution, is included in the bottom panel for comparison. The blue vertical lines show the location of the polarizing clouds identified with BISP-1; the red dashed vertical lines are the corresponding corrected distance (see Section 5.1). Bottom row: polarization orientation of stars in each cluster. The insets show the polarization angle distributions and the mean values (the red line). The black rectangle in the right panels indicates the approximate location of the IPS-GI field of view. The dark-blue pseudovectors represent the average orientation of the magnetic field within the region as observed by Planck.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top: LOSs of C5 (in yellow), C45 (in green), and C50 (in red) drawn over the extinction density XY plane from J. L. Vergely et al. (2022) at 10 pc (d < 1.5 kpc) and 25 pc (d > 1.5 kpc) resolutions. The markers indicate the adjusted positions of optical polarization clouds. Y. Doi et al. (2024)’s results for the Sagittarius Arm are displayed in blue for comparison. Bottom panels: G-band extinction from Gaia Collaboration et al. (2023) as a function of the photogeometric distance for all Gaia stars within C5 (top), C45 (middle), and C50 (bottom). The solid blue line is the median AG per distance bin. The vertical lines show the polarizing screens identified with BISP-1 using the optical (black) and NIR (orange) observations, corrected for the bias in the inverse parallax–distance relation (Section 5.1).
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Same description as in Figure 8, but for C45.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Same as in Figure 6 but using the NIR polarization observations. The black rectangle indicates the approximate location of the IPS-GI field of view.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Photogeometric distances from C. A. L. Bailer-Jones et al. (2021) as a function of the inverse parallax of the stars observed by IPS-GI and GPIPS in the regions of C5, C45, and C50. The solid gray line indicates the expected inverse parallax–distance relation. The shaded pink area represents the best fits of subsamples drawn without replacement from the measured data. The solid red line is the average best fit of the subsamples. The gray shaded area is the 2σ confidence intervals.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Same description as in Figure 8, but for C50.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: GMM results with optical (the two left columns) and NIR (the two right columns) polarization in C5 (top), C45 (middle), and C50 (bottom). The first and third columns are the group separations in normalized q−u space. The ellipses represent the Gaussian components. The second and fourth columns are the group membership probability as a function of photogeometric distance. The colors correspond to the components of Figures 8– 10.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top: comparison between the inverse parallax and the photogeometric distances from C. A. L. Bailer-Jones et al. (2021). Bottom: color–magnitude diagram from Gaia EDR3 photometry (Gaia Collaboration et al. 2021). Both panels present all high-quality Gaia measurements (i.e., ϖ/σϖ > 2, RUWE < 1.4, and ϖ > 0) in the region C5, colored by the parallax SNR, which saturates at 10. The red points represent faint stars with G > 18.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: Three examples of source deblending performed by PyBDSF. In each case, Blobcat had difficulty fully separating the five (left), four (middle), and three (right) sources in these examples. The white ellipse in lower right corner of each panel represents the synthesized beam size of the CHILES Con Pol.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: Catalog completeness as a function of the input S/N. The completeness is measured through Monte Carlo simulations and the error bars indicate 1σ uncertainty. Our catalog is complete 86% at 7σ and 96% at S/N = 15.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Left panel: our adopted priors for the temperature gradient, ﹩(d\mathrm{ln}T/d\mathrm{ln}P)﹩, at each of the 10 pressure layers evenly spaced in ﹩\mathrm{log}P﹩ from 103 bar (layer 1) to 10−6 bar (layer 10). Right panel: the 1σ/2σ/3σ (from dark to light blues) confidence intervals of the ﹩{(d\mathrm{ln}T/d\mathrm{ln}P)}_{{\rm{RCE}}}﹩ profiles computed from the Sonora Diamondback models. The black solid line represents the median ﹩{(d\mathrm{ln}T/d\mathrm{ln}P)}_{{\rm{RCE}}}﹩ profile, with black circles corresponding to the temperature gradient values at the 10 pre-defined layers. For pressures between 102 and 10−3 bar, we use orange lines to highlight the median values (solid), as well as the 1σ (dashed–dotted), 2σ (dashed), and 3σ boundaries (dotted) of our adopted Gaussian priors. For pressure layers with P < 10−3 bar or P > 102 bar, the adopted uniform prior is indicated by horizontal error bars.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Four schemes in our atmospheric inhomogeneity framework (Section 5.4).
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The archival JWST/NIRSpec spectrum (red) of 2MASS 1207 b, with the x-axis shown in log scale. Key atomic and molecular features are labeled. Several prominent accretion emission lines, identified by K. L. Luhman et al. (2023) and with detection significance values above 3.5σ (G.-D. Marleau et al. 2024), are highlighted in blue and are masked in our subsequent retrieval analysis.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Violin plot for the physical properties of 2MASS 1207 b inferred from its bolometric luminosity, age, and various evolution models (sorted by radii). The vertical dashed line inside each violin indicates the median value of the parameter, while the dotted lines represent the first and third quartiles of the distribution. Model labels and the parameter confidence intervals are summarized in Table 1.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Sketch of the temperature model described in Section 5.1.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The left column presents violin plots for the effective temperature, surface gravity, and radius of 2MASS 1207 b, as determined from thermal evolution models. These plots are based on the concatenated chains of parameters inferred from various evolution models (see Section 4.2). The right column presents the Teff, ﹩\mathrm{log}(g)﹩, and R values from all QEQ retrieval setups, following the same format as Figure 14.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-20, which assumes a homogeneous atmosphere with enstatite and iron clouds, with their base pressured determined from equilibrium chemistry (see Section 7.6.3). Evolution-based priors are adopted for ﹩\mathrm{log}g﹩, R, and M. These panels follow the same format as Figure 6.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-21, which assumes an inhomogeneous atmosphere with cloud-free hot/cold spots, along with broad priors for ﹩\mathrm{log}g﹩, R, and M (see Section 7.6.1). The middle-left panel presents the retrieved T–P profiles from individual atmospheric columns. These panels follow the same format as Figure 6.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The bolometric correction (specBCλλ; defined by Equation (A1)) for wavelength ranges of λλ = 1–2.4 μm (top), 1–5 μm (middle), and 6–13 μm (bottom), calculated using multiple grids of atmospheric models. The y-axis on the right presents the ratio between the integrated spectral luminosity over λλ and the bolometric luminosity, ﹩{L}_{\lambda \lambda }/{L}_{{\rm{bol}}}=1{0}^{-{{\mathtt{specBC}}}_{\lambda \lambda }}﹩. These plotted values are summarized in Tables 6, 7, and 8.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-9, which resembles the QEQ-13 setup (Figure 20) but adds a gray cloud component to the second atmospheric column (see discussions in Section 7.6.3). Evolution-based priors are adopted for ﹩\mathrm{log}g﹩, R, and M. These panels follow the same format as Figure 6.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-15, which resembles the QEQ-20 setup (Figure 18) but allows the cloud base pressures to vary as free parameters (see discussions in Section 7.6.3). Evolution-based priors are adopted for ﹩\mathrm{log}g﹩, R, and M. These panels follow the same format as Figure 6.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-13, which assumes an inhomogeneous atmosphere with patchy forsterite and iron clouds with hot spots (see discussions in Section 7.6.3). Evolution-based priors are adopted for ﹩\mathrm{log}g﹩, R, and M. These panels follow the same format as Figure 6.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieval results for QEQ-22, which assumes a homogeneous cloud-free atmosphere with broad priors for ﹩\mathrm{log}g﹩, R, and M (see Section 7.6.1). These panels follow the same format as Figure 6.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: TESS, follow-up, and archival observations of TOI-2844 compared to the the EXOFASTv2 results. Upper left: unbinned TESS and follow-up ground-based transits, phase-folded and shown in comparison to the best-fit EXOFASTv2 model with an arbitrary normalized flux offset. Multiple TESS sectors in the same cadence are stacked on top of each other. Bottom left: the SED of the target star compared to the best-fit EXOFASTv2 model. Residuals are shown on a linear scale, using the same units as the primary y-axis. Upper right: RV observations vs. time, including any significant long-term trend. The residuals are shown in the subpanel below in the same units. Middle right: RV observations phase-folded using the best-fit ephemeris from the EXOFASTv2 global fit. The phase is shifted so that the transit occurs at phase + offset = 0. The residuals are shown in the subpanel below in the same units. Bottom right: the evolutionary track and current evolutionary stage of the primary star according to the best-fit MIST model. The blue line indicates the best-fit MIST track, while the gray shaded contours show the 1σ and 2σ constraints on the star’s current Teff and ﹩\mathrm{log}g﹩ from the MIST isochrone alone. The green contours represent the 1σ and 2σ constraints on the star’s Teff and ﹩\mathrm{log}g﹩ from the EXOFASTv2 global fit, combining constraints from observations of the star and planet. The red cross indicates the median and 68% confidence interval.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: The AO images and contrast curves for TOI-4462 and TOI-5240 taken by PHARO on the 5.0 m Palomar telescope. Left: TOI-4462 in the Kcont filter with a bright companion clearly seen at a separation of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩4. Right: TOI-5240 in the Brγ filter with a faint companion at a separation of 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩4.