adsabs/AstroCLIMB huggingface dataset:
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Distribution of the fractional difference f between systems located within the i = 80°–100° bin and those located in the i = 0°–20° or i = 160°–180° bins in Figure 7. The dark blue histogram is comprised of the same 30,000 random draws used to produce the error bars in Figure 7. Based on the distribution of f, the “strict” sample is more centrally peaked toward an edge-on distribution rather than an isotropic distribution at the ∼3σ level.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Distance distribution of HZ planet populations around M and FGK-type stars detectable with LIFE in the current baseline setup (see Table 1). Left: Detection yield predictions for planets around M-type stars with an underlying AFGKM exoplanet population following occurrence rate estimates from NASA’s ExoPaG SAG13 (Kopparapu et al. 2018) and Dressing & Charbonneau (2015). Right: Detection yields predictions around FGK-type stars with an underlying FGK exoplanet population based on the occurrence rates from Bryson et al. (2021). We differentiate between three HZ definitions: optimistic (opt) HZ, conservative (con) HZ, and EECs. The bars show the predicted median planet yields and 1σ uncertainties derived from the Monte Carlo simulations.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various fluxes of N2O in the emission spectrum of an Earth-like planet around a (from top left to bottom right:) Sun-like, K6V, Proxima Centauri-type, and Trappist-like star at 5 pc, after 50 days of observation with LIFE. Top: planet flux for atmospheres with and without N2O. The gray area represents the 1σ sensitivity; the dark gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between atmospheric models with and without N2O. For the Sun-like case, the main contribution to the detectability is in the 16–18 μm band. For the later-type star cases, the differences are especially in the 8–9 μm band (see also the discussion in Section 4.1).
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various levels of CH3Cl and CH3Br fluxes in the emission spectrum of an Earth-like planet around a Proxima Centauri-type star, after 50 days of observation with LIFE. Top: planet flux for atmospheres with and without CH3Cl and CH3Br. The gray area represents the 1σ sensitivity; the gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between an atmospheric model with and without CH3Cl and CH3Br.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Comparison of stellar properties in the HPIC (x-axes) and ExEP HWO precursor science list (y-axes). Uncertainties are plotted when available, though note that for a few properties and individual stars, uncertainties are not available from both catalogs. Stellar properties are consistent between these two catalogs, excluding one or two outliers.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Residuals between HPIC and ExEP values of stellar properties. Note that fractional residuals are shown for all quantities except log(L), [Fe/H], and log(g), where differences are shown. Single outliers have been omitted in a few subplots in order to make the distribution of residuals clearer to see.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Comparison of the stars selected for a 2 yr EEC survey using the baseline AYO input catalog and the updated HPIC. Points are color coded by HZ completeness. Details about the different yield calculations are given in Table 3. The population of stars selected does not change significantly when updating the target list, but the completeness of individual stars and their relative priority can change.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Histogram of stellar properties for stars in the HPIC. Note that a few outlier stars fall outside the axis range of some of the histograms. Surface gravity shown here is log(g) calculated using stellar bulk properties.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Distribution of TESS magnitudes for TIC objects within 50 pc. The black vertical line shows our magnitude cutoff at 12, which maintains volume completeness.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Stars selected for a 2 yr EEC survey using an 8 m inscribed diameter “Super LUVOIR-B” telescope. Points are color coded by HZ completeness. About twice as many stars as the baseline LUVOIR-B case are selected, extending to larger distances.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Diagram illustrating the procedure used to construct the HPIC.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Scatter plots of Stokes parameters q (top panel) and u (middle panel) vs. distance for all fields. The bottom profiles show the differential extinction (or extinction density) in mag kpc−1 taken from Lallement et al. (2022) and Vergely et al. (2022). The dotted and dashed vertical lines in the scatter plots of fields C11 and C15 indicate the average distance of the nearby and distant populations, respectively. The turnover point at which the polarized signal changes occurs at a distance of approximately 1.3 kpc.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Distributions of Stokes parameters q and u and distance d in kpc. Top: field C11. Red and blue indicate the nearby and distant partitions, respectively, created using DBSCAN. Gray indicates data points that are not part of either component; see also Section 4.1. Bottom: field C15. Red and blue indicate the nearby and distant partitions, respectively, created using K-means clustering; see also Section 4.2.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Distance-normalized extinction (A  V /dist) vs. distance for ∼2.5 million stars in the general area of the Southern Coalsack. Data taken from Anders et al. (2022). Red data points are the individual stars, the gray background indicates the 25%–75% quantile range, and the black solid line indicates the median. The increase in A  V /dist is caused by the presence of the Coalsack at a distance of ∼185 pc. The inset shows a Gaussian fit to the A  V /dist excess. We estimate an LOS thickness of 25.7 ± 0.6 pc.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top left: the square root of the structure function of the polarization angles (the ADF; see Equation (6)) of the nearby population of field C15. The red line indicates the best fit to the first five bins. Top right: polarization vector plot of the nearby stars of field C15. The red marked star indicates an observation removed from further analysis. Bottom left: the ADF (Equation (6) of the polarization angles of the nearby population of field C11. Bottom right: polarization vector plot of the stars in the nearby population of field C11.
Paper: Magnetic Fields in the Southern Coalsack and Beyond
Authors: M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata
Figure caption: Per field, for each star its polarization angle and distance. Distances taken from Anders et al. (2022). The dotted lines indicate the average magnetic field orientation at the location of the center of the field taken from the Planck 353 GHz HFI maps. The shaded area shows the uncertainty of the Planck polarization angle.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Velocity fields of MCs with double 13CO structures, whose relative velocities are characterized as distinct velocity discontinuities. Left panel: The color map represents the first-moment map (velocity field) of 12CO emission of MCs, and the cyan contours show the moment-zero map (velocity-integrated intensity) of 13CO line emission, ranging from 10% to 90% in increments of 20% of its maximum value. Middle panel: The color map represents the first-moment map (velocity field) of 13CO emission of MCs, and the cyan contours show the moment-zero map (velocity-integrated intensity) of 12CO line emission, ranging from 10% to 90% in increments of 20% of its maximum value. Right panel: The averaged spectral lines for the extracted 12CO line emission (black) and 13CO line emission (cyan) within MCs. The number noted in the upper-left corner is the number ID for MC samples.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Number distributions of angular areas, velocity spans, integrated fluxes, and peak intensities of 12CO line emission for MC samples in the near group. Most of these samples are located in the Local Arm and have kinematical distances of ∼0.5 kpc. The gray histograms represent 163 12CO MCs with double 13CO structures, and the green histograms represent 80 12CO MCs with triple 13CO structures.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Number distribution of angular areas, velocity spans, integrated fluxes, and peak intensities of 12CO line emission for MC samples in the far group, most of which are distributed in the Perseus arm with kinematical distances of ∼2 kpc. The gray histograms represent 280 12CO MCs with double 13CO structures, and the green histograms represent 105 12CO MCs with triple 13CO structures.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Same as Figure B1, but for the MC with triple 13CO structures, where three distinct velocities discontinuities between each two of 13CO structures are determined.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Same as Figure B1, but for the MC with triple 13CO structures, where two distinct velocity discontinuities between each two of 13CO structures are determined.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Top panel: dust luminosity per area vs. mass of the young stellar population per area. Middle panel: average dust luminosity per area vs. distance in 1 kpc bins, with errors given by standard deviations of each bin. Peaks are seen at 5 and 11 kpc. Bottom panel: dust.qpah vs. distance. The average dust.qpah is similar to the average value given by Draine et al. (2014), but the errors are significantly larger here, so that a distance dependence is not seen here.
Paper: Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31
Authors: Denis A. Leahy, Jakob Hansen, Andrew M. Hopkins
Figure caption: Top panel: mass of the old stellar population per area vs. distance of each region. The red line shows the best-fit function, with parameters given in Table 2. Middle panel: tau_main (old stellar population) vs. distance and best-fit function. Bottom panel: mass of the young stellar population per area vs. distance and best-fit function.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Subplots for the Cygnus X North region. Panel (a) shows 13CO (white contours in [5, 20, 35, 50] × σ, σ is the noise level of intensity map) and C18O (colormap) emission in [−9, 1] km s−1. Massive star-forming regions are sited along the dense filamentary structure, i.e., DR21, DR23, and DR22. Black contours also denote the dense molecular gas in [7, 12] km s−1 in same levels, e.g., W 75N is overlapped on the DR21 filament. Some H II regions are marked with triangles. The extent of Cygnus OB2 is plotted in a white circle. Distances with 5% system error of our measured clouds and those from masers are presented; different gas layers are also labeled with different colors. Panel (b): the gray-scale map is 13CO emission from velocity interval of [−9, 1] km s−1, overlaid with smoothed data from [1, 7] km s−1 (white contours in [2, 6, 10, 14, 18, 22] K km s−1). Panel (c): all the same with panel (b), but contours for velocities in [7, 20] km s−1. Panel (d): a moment 1 map of centroid velocities extracted from Gaussian decomposition for clouds in [−9, 1] km s−1. Obviously, prominent velocity gradient along filamentary structure can be seen. Panel (e): an 8 μm Midcourse Space Experiment (MSX) image toward the Cygnus X North region (Egan et al. 1998). Gray edged rectangles mark the identified molecular cloud with the associated mid-IR features. The extent of these rectangles is derived from the ±3σ of v, l, b relative to cloud center in Table 3. Panel (f): a 1030 pc slice of 3D dust map from Bayestar 2019 (Green et al. 2019), overlaid with the 1 kpc MC layer (red contours) from our samples (class I in Table 1) with well-determined distances. Note that our results are in good agreement with Green et al. (2019).
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Subplots toward the Cygnus X South region. Panel (a): 13CO (white contours in [5, 10, 20, 35, 50, 70]×σ, σ is the noise level of intensity map) and C18O (colormap) emission in [−3, 3] km s−1. These H II regions and dense cores of L889 are marked with triangles. The extent of OB associations and SNRs are plotted in yellow ellipses. Distances (with 5% system error) of our measured clouds and those from masers are also presented. Panel (b): moment 1 map in [−3, 3] km s−1. Panel (c): the gray-scale map is 13CO emission from [−3, 3] km s−1, overlaid with smoothed data from [3, 12] km s−1 with levels [10, 25, 40, 55, 70, 85]×σ. Panel (d): all the same with panel (c), but contours for velocities in [−10, −3] km s−1. Panel (e): same with Figure 8e, but for Cygnus X South region. Panel (f): a 918 pc slice of 3D dust map from Bayestar 2019 (Green et al. 2019), overlaid with L889 cloud at ∼935 pc (red contour) from our samples (see cloud 57 in Table 1).
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Physical properties of clouds in the Cygnus X South region. Panel (a): 13CO peak temperature of MCs. Different colors are marked for clouds in different gas layers. Clouds in background layer (blue dots) are all associated with bright mid-IR features. Clouds in filled dots have cometary or globular morphology, which is a strong evidence that has been shaped by massive OB star groups, e.g., cloud A, B marked by Schneider et al. (2006), while clouds in empty dots are oval shaped or irregular, e.g., DR6 and DR9. Panels (b) and (c): the same with panel (a), but show velocity dispersion and column densities of the clouds.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Left panel: Our results for 120 robust distance measurements both in Models A and B (class I, see details in Section 4.3). We find that all differences between Model A and Model B are smaller than 150 pc, except cloud G76.74–0.43 (ID 30 in Table 1). Right panel: LTE mass statistics based on our cloud catalog, i.e., black histogram from samples of class I in Table 1, gray histogram with slashes included class II results from Table 1, while blue and red histograms from Tables 2 and 3.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: 3D plot of different gas layers toward the Cygnus X North region. Panel (a): Scatter plot of clouds in background layer (i.e., 1.3 ∼ 1.7 kpc). Colors mark different 13CO structures identified by ACORNS, and each dot presents pixel-by-pixel centroid velocities. Their summed intensities are projected at the bottom. Panel (b): Scatter plot of clouds in 800 and 1 kpc layers. Clouds in 800 pc are in orange, while clouds in 1 kpc are in cyan. Both of the two layers display large filamentary complexes overlapped together. Clouds in 1.3 ∼ 1.7 kpc layer are also plotted as colored contours on the bottom, which shows the spatial relation of different clouds on projection.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Physical properties of clouds in the Cygnus X North region. Panel (a): 13CO peak temperature of MCs. Different colors are marked for clouds in different layers. Clouds in background layer are associated with masers or bright cometary mid-IR features (filled blue dots) and the nearby dense gas structures (empty dots) along the filamentary structure of Cygnus X North star-forming region. Panels (b) and (c): the same with panel (a), but for velocity dispersion and column densities of the MCs.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Panel (a): Measured distances of different 13CO structures toward the NAP region. Black line and blue shadow show the averaged distance and dispersion (without the 5% system error) weighted by clouds' masses. Panel (b): distances compared to Zucker et al. (2020) with labeled 5% system error (gray shadow) relative to distance; a systematic deviation can be found (see details in Section 4.3).
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: The same as Figure 5, but for cloud G76.74-0.43 (ID 30 in Table 1). The fluctuation of A  G –Distance relation for on-cloud stars for Model A denotes worse baseline fitting. We thus choose the result from Model B (see Section 4.2.2).
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Panel (a): 13CO (white contours in [10, 20, 30, 45, 60, 75, 90] × σ, σ is the noise level of intensity map) and C18O (colormap) emission in [−10, 10] km s−1 toward the NAP region. Panel (b): a 3D plot for all 13CO structures with measured distances in the region.
Paper: Validation of a Third Planet in the LHS 1678 System
Authors: Michele L. Silverstein, Thomas Barclay, Joshua E. Schlieder, Karen A. Collins, Richard P. Schwarz, Benjamin J. Hord, Jason F. Rowe, Ethan Kruse, Nicola Astudillo-Defru, Xavier Bonfils, Douglas A. Caldwell, David Charbonneau, Ryan Cloutier, Kevin I. Collins, Tansu Daylan, William Fong, Jon M. Jenkins, Michelle Kunimoto, Scott McDermott, Felipe Murgas, Enric Palle, George R. Ricker, Sara Seager, Avi Shporer, Evan Tey, Roland Vanderspek, Joshua N. Winn
Figure caption: Ground-based transit observations of LHS 1678 b in order of their acquisition. Colored points and error bars trace individual, discrete photometric measurements. The white-filled black circles represent the measurements binned to a 10 minute interval. The black lines trace the best-fit model with dashed, dotted, and dotted–dashed lines distinguishing between planets b, c, and d, respectively, in the case of multiple planet transits. The observatory used and date of observation are listed next to each light curve in the same color as the observed data. Light curves taken on 2019 July 27, 2019 December 14, 2021 November 15, 2021 November 18, and 2022 January 1 feature transits of multiple planets, including a partially overlapping transit with LHS 1678 d on 2022 January 1.