adsabs/AstroCLIMB huggingface dataset:
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Distribution of Lagoon Nebula YSOs according to their accretion properties (as traced via E(r − Hα)CCD, Section 5.2) vs. disk properties (as traced via α IRAC, Section 3.2). The colors and symbols denote the final accretion/disk classifications derived for each object from our analysis: small gray dots are stars without evidence of accretion from all available indicators, blue dots are accreting sources, red crosses are potential accretors, black squares surround disk-bearing sources, and green triangles surround disk candidate sources. The disk class labels at the top of the figure follow the α IRAC scheme by Teixeira et al. (2012).
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Example of a periodic K2 light curve for a young accreting star in the Lagoon Nebula (top) and results of the correlation analysis between the K2 time series and each of the u, g, r, i light curves as a function of the hypothetical time lag between the respective variation patterns (bottom), as described in the text. The overlaid curves in the bottom panel represent sinusoidal fits to the measured (Δt, ρ) trends.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Left panel: jackknife stack of 24 (60 s) frames of the 2020 Keck OSIRIS K  p  band follow-up observation. Upper right panel: close-up (2.″5 × 2.″5) frame of the source and lens. Lower right panel: close-up (2.″5 × 2.″5) of the two-star PSF fit residual using DAOPHOT.
Paper: A Pan-STARRS1 Search for Planet Nine
Authors: Michael E. Brown, Matthew J. Holman, Konstantin Batygin
Figure caption: The combined V-band magnitude limits of the ZTF, DES, and PS1 suerveys for Planet Nine, reconstructed from detections of the synthetic reference population. The geometry is the same as Figure 1. Note that the sky area is smaller than in Figure 1 because we require a minimum of 4 members of the reference population to be present to estimate a limit. The deep DES survey on the far right has magnitude limits that extend as far as 24. The areas in dark blue remain unsurveyed.
Paper: A Pan-STARRS1 Search for Planet Nine
Authors: Michael E. Brown, Matthew J. Holman, Konstantin Batygin
Figure caption: The V-band magnitude at which there is a 95% or higher probability that a moving object would be detected 9 or more times in the portion of the PS1 data that intersects the predicted locations of P9. The data are shown in a Mollweide equal area projection in equatorial coordinates. R.A. of 360 is on the left with 180 in the middle and 0 on the right. The ecliptic is indicated by a line, as well as galactic latitudes of ±15°.
Paper: A Pan-STARRS1 Search for Planet Nine
Authors: Michael E. Brown, Matthew J. Holman, Konstantin Batygin
Figure caption: The probability density function of on-sky location of the BB22 Planet Nine reference population that would remain undetected after the ZTF, DES, and PS1 surveys. The geometry is the same as Figure 1.
Paper: A Pan-STARRS1 Search for Planet Nine
Authors: Michael E. Brown, Matthew J. Holman, Konstantin Batygin
Figure caption: The fraction of the BB22 Planet Nine reference population that would have been detected by the ZTF, DES, and PS1 surveys, as a function of V-band magnitude. The combined surveys are extremely efficient for objects fainter than V ∼ 21 and reach 50% efficiency at V = 21.5, with a large tail of fainter detections from the deep but narrow DES survey.
Paper: The Long-term Activity of the Postnovae Q Cygni and BK Lyncis
Authors: Vojtěch Šimon
Figure caption: (a) Light curves of superoutbursts in postnova BK Lyn (CCD data). The individual events were shifted along the time axis to match the rising branch of the template (circles) in crossing 14.5 mag (times of this crossing and the shifts are given). A horizontal dashed line marks a crossing of this line. The filled symbols denote the night means, while the empty symbols mark the isolated observations. The error bars of the night means are sometimes comparable to the size of the symbols. The individual events were connected by the line to guide the eye. (b) A segment of the light curve of BK Lyn between superoutbursts. The night means and their error bars are plotted. A horizontal line near JD 2 456 000 marks a remarkably long decay of a probable superoutburst. (c) The light curves of the well-covered decaying branches of outbursts of BK Lyn. The individual outbursts were shifted along the time axis to match the decaying branch of the template (empty squares). The time of crossing 15.5 mag of each event is marked. All normal outbursts reach similar decay rates after crossing the dashed vertical line (only a decline of a probable superoutburst (empty circles) joins later). A linear fit to the ensemble and its statistical deviation is displayed. The lines and numbers at the edge of the panels represent M opt for d and A  V  of BK Lyn. See Section 4 for details.
Paper: The Long-term Activity of the Postnovae Q Cygni and BK Lyncis
Authors: Vojtěch Šimon
Figure caption: (a) The long-term activity of postnova BK Lyn from 1890 to 2023. (The photographic DASCH, CCD CRTS, and CCD AAVSO data). The error bars are marked. A linear fit and its standard deviation are included. The lines and numbers at the edge of panel (a) represent M opt for its d and A  V . (b) Detail of the segment with outbursts and its surroundings. (c) Histogram of M opt of BK Lyn. Notice the prominent tail of the S1 and S2 time segments. (d) Parameters of the outburst light curves of DNe with P orb similar to BK Lyn (mostly superoutburst peaks and quiescent M opt). The vertical long dashed lines in panels (c) and (d) represent a combination of the outburst and superoutburst peaks of DNe analyzed by Patterson (2011), appropriate to P orb of BK Lyn (the short dashed lines denote its standard deviation). See Section 4 for details.
Paper: A Revisit of the Mass–Metallicity Trends in Transiting Exoplanets
Authors: Qinghui Sun, Sharon Xuesong Wang, Luis Welbanks, Johanna Teske, Johannes Buchner
Figure caption: The mass–metallicity correlation among planets, with the x-axis representing planet mass in Jupiter masses (M J) and the y-axis denoting normalized planetary abundance, both are in logarithmic scales. Our normalized H2O abundances are denoted by blue open circles, while the solid blue line represents the best-fit linear regression. The shaded blue region delineates the 1σ and 2σ quantiles. The trend depicted in W19 is shown by the dotted blue line, which exhibits a slightly more significant slope than ours. The linear model in our analysis is expressed as log(H2O) = −0.92﹩{}_{-0.33}^{+0.32}﹩log(M/M J) − 0.90﹩{}_{-0.20}^{+0.21}﹩. A recent detection of H2O from JWST/NIRISS for HAT-P-18b (Fu et al. 2022) is shown in the light purple circle in Figure 2.
Paper: A Revisit of the Mass–Metallicity Trends in Transiting Exoplanets
Authors: Qinghui Sun, Sharon Xuesong Wang, Luis Welbanks, Johanna Teske, Johannes Buchner
Figure caption: [C/H], [O/H], and C/O ratios plotted against [Fe/H] for our planet-hosting stars using spectra from HARPS, FEROS, and HIRES. The blue open circles show C and O abundances for planet-hosting stars from Nissen (2013), while the light purple and gray open circles show planet-hosting and non-planet-host stars, respectively, from Delgado Mena et al. (2010). The background stars in our study exhibit a T eff range of approximately 5000–6500 K, whereas our stars have a much broader T eff range spanning from 3500 to 7500 K. The error bars are combined from σ  μ  and error propagated from stellar atmospheres. In the works of Nissen (2013) and Delgado Mena et al. (2010), errors for individual stars are not provided. Instead, they estimate typical σ  μ  to be around 0.1 dex and 0.2 dex for [C/H] and [O/H], respectively.
Paper: A Revisit of the Mass–Metallicity Trends in Transiting Exoplanets
Authors: Qinghui Sun, Sharon Xuesong Wang, Luis Welbanks, Johanna Teske, Johannes Buchner
Figure caption: This figure compares the linear regression model (top panel) and the independent distribution model (middle panel) for H2O, Na, and K. The 1σ and 2σ quantiles are shown in the color-shaded region. The bottom panel displays the Monte Carlo simulation distributions, which were generated by performing 200 tests using the 10,000 data points generated from the linear correlation. We depict the K = 101/2 line, none of the distributions indicate substantial or strong evidence favoring the linear model over the constant model.
Paper: A Revisit of the Mass–Metallicity Trends in Transiting Exoplanets
Authors: Qinghui Sun, Sharon Xuesong Wang, Luis Welbanks, Johanna Teske, Johannes Buchner
Figure caption: The normalized planetary atmosphere H2O, Na, K abundance vs. other planetary/stellar parameters.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: PV maps along the arrow line shown in Figure 5(b). The top two panels depict the 12CO emission, while the bottom two panels display the 13CO emission. The 12CO contours start at 1 K and increase in steps of 1 K (σ ∼ 0.3 K). The 13CO contours start at 0.3 K with an increasing step of 0.6 K (σ ∼ 0.1 K). The blue dashed lines in the first and third panels indicate the velocity ranges, which are magnified in the second and fourth panels, respectively. The red dashed line shows the “by-eye” fitting of sine waves to the oscillating velocity dispersion, with an oscillation period of T ∼ 1.4 pc. The vertical arrow lines mark the positions of striations according to the local peaks of the 12CO emission (see Figure 6).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: POS magnetic field overlaid on the MWISP 13CO integrated intensity map. The colorful background shows the 13CO emission, integrated over the velocity range of 0–6 km s−1. The “drapery” pattern, produced with the line integral convolution method (Cabral & Leedom 1993), indicates the orientation of magnetic field lines derived from Planck dust polarization data. The colorful contours show three subregions with different polarization PAs (see Figure 11).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption:  12CO striations revealed in different velocity channels. The striations found in the [4, 6] km s−1 velocity range are located in the central part of the L914 cloud, while the striations in [0, 2] km s−1 are situated in the western region. The blue solid line shows part of the dense ridge related to the striations, which is identified with the DisPerSE algorithm. The green rectangle demonstrates the slice used for intensity profile plotting (see Figure 6). The magenta arrow line shows the path used for the PV map (see Figure 7).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Profiles (blue solid lines) of averaged intensity along the directions perpendicular to the striations (magenta arrow lines in Figure 5). The orange dotted line shows the profile after applying a low-pass noise filter. The green and red dots represent the local maxima and minima, respectively.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Velocity-integrated channel maps of the 12CO (grayscale background), 13CO (lime contours), and C18O (magenta contours) line emission. The integrated velocity range is marked in the bottom right corner of each panel in units of km s−1. The 13CO contours start at 1 K km s−1 and increase with a step of 1 K km s−1 (σ ∼ 0.15 K km s−1). The C18O contours start at 0.5 K km s−1 and increase by 0.5 K km s−1 (σ ∼ 0.15 K km s−1).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption:  13CO narrow velocity-integrated integral maps of the striations. The grayscale backgrounds represent the integrated intensity of the 13CO emission with integrated velocity ranges of [4.5, 5.1] and [1.5, 2.4] km s−1, respectively. The contour levels are at 0.75, 1.5, and 2.25 K km s−1 (σ ∼ 0.25 K km s−1). Striations S1–S6 (see Section 3.1) are shown with red dotted lines. The blue solid line represents the dense ridge (the same as Figure 5).
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: Velocity-integrated intensity maps of 12CO, 13CO, and C18O (from top to bottom) toward the L914 cloud. The integral interval is labeled at the top right corner of each panel. The cyan line in each panel represents the ridge of the L914 filamentary cloud identified by the DisPerSE algorithm using the C18O data.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: CO PV image along the ridge of the L914 filamentary cloud (from east to west). The grayscale background represents the 12CO emission. The lime and pink contours represent the 13CO (levels = 0.75, 1.75, 2.75 K; σ ∼ 0.15 K) and C18O (levels = 0.5, 1.0, 1.5 K; σ ∼ 0.15 K) emission, respectively.
Paper: Magnetically Aligned Striations in the L914 Filamentary Cloud
Authors: Li Sun, Xuepeng Chen, Min Fang, Shaobo Zhang, Yan Gong, Jiancheng Feng, Xuefu Li, Qing-Zeng Yan, Ji Yang
Figure caption: H2 column density map calculated with the 13CO emission. The blue contours show the density levels of 1, 3, 5, and 7  ×  1021 cm−2. The cyan contours show the C18O integrated intensity with levels at 0.3, 0.9, 1.5, and and 2.1 K km s−1. The purple, orange, and lime lines represent the segments in Section 3.3.1.
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: The distance measurement of cloud G084.88–0.20 (ID 185 in Table 1) from Models A and B. The Gray-scale map in the left side presents the 13CO integrated intensity of the cloud and its neighbors. Black contour plots the MC structure identified with ACORNS based on the Gaussian decomposition, while white contour expands the MC structure boundary with 5′. All on-cloud stars located within the cloud are marked as red dots, while referenced stars (blue dots) are chosen out of white contour; see details in Figure 4. Corner plot in the upper right gives the MCMC sampling results from emcee. We set three parameters in our model, nwalker = 50, the number of burn-in samples for Markov chain with 1000, and steps with 2000. All binary relations among parameters are presented as 2D Gaussian distributions. We compute median value (solid line) of all samples for result, and 1σ confidence interval in dashed lines (16th and 84th percentile). Subplot in the lower right presents an A  G –Distance relation for on-cloud stars. The upper one gives A  G  values before baseline elimination, while the lower one gives the result by subtracting a monotonous fitting of reference stars (see Section 4.2.2). Gray dots are raw data from Gaia DR3, while red and blue dots are binned values in a 10 pc interval for on-cloud and off-cloud stars, respectively. Orange vertical lines denote all the jump points in MCMC sampling. Model A give a significant jump, and it matches better with distances in literature of NAP region.
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 sketches illuminate our method based on BEEP (Yan et al. 2019a). On-sources are selected within the 13CO structure. (a) Use 12CO emission to choose field stars. (b) Use 13CO from its own morphology to select field stars in its periphery. Red region is the identified 13CO cloud, which is partly overlapped by a neighboring cloud in green. The black part is the region with superposition, which include more than one Gaussian component. White solid contour and black dashed contour denote different dilation of cloud boundary. Orange part represents the reference region. Blue area represents the widespread 12CO emission. Obviously, Model A considers the 12CO free region as the reference region, while Model B refers to 13CO morphology to select the reference stars (see Section 4.1.2).
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: (a) Reconstruction of moment 0 map of 13CO emission; the values in gray scale are fluxes summed up by all Gaussian components in each sight line. (b) Similar to (a), but only for the emission with Gaussian components after clustering. (c) Reconstruction of moment 1 map, showing the centroid velocity of Gaussian components. We choose most positive velocities on the top (top positive), but not a weighted average. (d) The same with (c), but smallest velocities on the top (top minus). (e) The moment 2 map, showing the line width of most positive velocities on the top. (f) The same with (e), but smallest velocities on the top. (g) The distribution of the number of Gaussian components in the whole region. And (h) the residuals between integrated emission of raw data and reconstructed image by Gaussian decomposition.
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: A composite guide map colored in R (C18O), G (13CO), B (12CO) based on the MWISP data. The map is made by moment masking method. That is, pixels with three continuous channels beyond 3 times that of the noise level have been kept. Many prominent structures are denoted on this map, including OB associations and SNR γ Cygni (labeled with large circles or ellipses), dark clouds (triangles), and radio sources (white small circles) collected by Downes & Rinehart (1966), as well as several H II regions (yellow circles). The light green rectangles indicate some interesting subregions discussed in Section 5.
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 average spectrum of 13CO toward the Cygnus region. Gray line shows the raw data truncated from −100 to 50 km s−1, while black line denotes the average spectrum after resampling. Blue curve indicates the average of all signals restored by Gaussian decomposition, while red line shows the average spectrum after clustering based on ACORNS (Henshaw et al. 2019). Toward the Cygnus region, we note that a collective cloud emission overlapped together within a narrow velocity range (−20 to 20 km s−1). The flux reconstructed by Gaussian decomposition and clustering are 81.5% and 79.5% (see Section 3.3), respectively.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: The vertical axis indicates the ratio (raw contrast) of the stellar and planetary throughputs including the fiber-coupling efficiency. The horizontal axis means the stellar angular diameter normalized by λ  c /D. The markers indicate the simulation results with the assumption that (θ  x , θ  y ) = (1.125, 0.750). The colors of markers mean the difference in spectral bandwidths (see the legend). The dashed straight lines connect the markers as interpolation.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: The color map in the left panel shows planetary throughputs (including fiber-coupling efficiencies) in the case of different angular separations; the horizontal and vertical axes indicate the x- and y-directional separation angles normalized by λ  c /D, respectively. The calculation for the left panel assumes a monochromatic light source (Δλ/λ  c  = 0). The horizontal axis of the right panel indicates the spectral bandwidth Δλ/λ  c . The vertical axis of the right panel denotes the planetary throughput including the fiber-coupling efficiency. The markers in the right panel show the simulation results; the red and black markers indicate the case when the planetary separation angles (θ  x , θ  y ) = (1.125, 0.750) and (θ  x , θ  y ) = (1.000, 1.000), respectively. The dashed straight lines connect the markers as interpolation.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: A schematic showing how planetary light can transmit the single-mode fiber located at the optical axis. The blue and red lines before the Lyot plane indicate off-axis planetary and on-axis steller light rays, respectively. The Lyot-stop phase-modulation mask (see also Figure 2) works as a two-dimensional diffraction grating, which creates multiple diffraction peaks on the next focal plane. We show the rays belonging to the four diffraction peaks with the diffraction orders (1, 1), (−1, 1), (1, − 1), and (−1, − 1) using different colors for every diffraction peak. When the planet has proper separation angles depending on mask parameters, one of the diffraction peaks exists near the optical axis and transmits the single-mode fiber effectively.
Paper: Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph
Authors: Satoshi Itoh, Taro Matsuo, Motohide Tamura
Figure caption: A block diagram showing how the new concept eliminates undesirable leakage amplitudes. See the main text for definitions of EE, EO, OE, and OO components. The red prohibited symbols mean that the associated components fail to transmit the single-mode fiber.