adsabs/AstroCLIMB huggingface dataset:
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Spectra of the [C II], [O I], CO(J = 6-5), and CS lines toward the three brightest [O I] positions. The lower-right three panels show the absolute spectra in degrees kelvin. The upper-left three panels show the same spectra normalized to their maxima. Half-maximum, for estimating the FWHM, is marked with dashed horizontal lines. The [C II] spectra are shown after the spectral background subtraction described in Appendix B, and the unsubtracted [C II] spectra are shown with dotted lines in the lower-right panels for context. Vertical lines mark every 1 km s−1 between 20 and 27 km s−1. The [O I], CO, and CS observations are all convolved to the [C II] beam, shown in the lower-right corner of the central panel. The central panel shows [C II] (color) and [O I] (contour) emission integrated between 20 and 27 km s−1. The [O I] contours are placed at [0, 6, 12, 18, 24, 30] K km s−1. Dashed gray lines in the central panel show the area covered by these [O I] observations. Velocities are relative to the local standard of rest (LSR).
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: HCO+ (color) and CS (contour) line channel maps binned to 1 km s−1 and centered on the Pillars. The HCO+ images use an arcsinh color scale to make low-level emission more visible. The CS contours mark [0.7, 4.7, 8.7] K. The contour colors are chosen to increase contrast with the image and have no further significance. The CS (left) and HCO+ (right) synthesized beams are shown in the lower-right corner of each map. The HCO+ (CS) 50% gain contour is shown with a dashed (dotted) line.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: 158 μm [C II] line channel maps binned to 1 km s−1 and centered on the Pillars. The beam is shown in the lower-right corner of each map.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption:  Sine morte stellar mass distributions (left) and ISO water mass fraction distributions (right), integrated over z, at each distance to the Galactic center R. Both distributions are normalized such that at each value of R the integral over [Fe/H] or ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ is unity. Dashed lines show the median value of each distribution at each R.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: Distribution of ISO water mass fractions, evaluated at the position of the Sun and integrated over the Milky Way disk, with maximum a posteriori estimate of β = 1.33. At ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}=0.3﹩ a vertical line marks the measured water mass fraction of 2I/Borisov.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: Alternate prediction for the distribution of ISO water mass fractions, evaluated at the position of the Sun and integrated over the Milky Way disk with β = 0: assuming the number of ISOs produced by each star is independent of the star’s metallicity.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: The expected (left panel) and observed (right panel) G − J excess as a function of ∣ΔG∣ between a Gaia eDR3 star and its low-separation neighbor. For the expected excess, the expected photometry from Pecaut & Mamajek (2013) is used to create the black data points. Here, the excess is defined as the difference between the G − J color with the 2MASS photometry artificially blended and the expected G − J color from Equation (7) based on the artificially blended BP − RP color for the sources. For the observed excess, we define the excess as the difference between the observed G − J color and the expected G − J color based on the star’s BP − RP color (Equation (7); (G − J)0). The dashed red line is an exponential function fit to the expected G − J excess data, where the expected relation matches the observed relation well.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Color–color diagrams of G − J vs. BP − RP for the 200 pc Gaia eDR3 sample cross-matched with 2MASS. The left panel shows all stars that have no Gaia eDR3 neighbor within 2.″5. The middle and left panels show stars than have a close neighbor within 2″ listed in Gaia eDR3. The black density map in each panel is on the same logarithmic scale. The red-dashed line is a second degree polynomial fit to the stars that have no Gaia eDR3 neighbor within 2.″5, where the fit was completed over 20 σ-clipped iterations. The colored dashed lines overlaid on the right panel show the expected color–color relation for binary systems with various mass rations, q, where colors were estimated using expected colors per spectral class from Pecaut & Mamajek (2013). When estimating expected colors, it is assumed that the Gaia G photometry is only from the resolved, more massive star while the Gaia BP and RP, and 2MASS photometry is blended from both sources.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: The expected G − J excess for WD–MS binaries. Here, white dwarf photometry from Gentile Fusillo et al. (2021) is combined with random samples of photometry from Pecaut & Mamajek (2013) and bootstrapped over 100 iterations to get the average distribution shown. The dashed red line is an exponential function fit to the expected excess from MS+MS binaries, as shown in the left panel of Figure 4.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: The observed G − J excess as a function of ∣ΔG∣ between a Gaia eDR3 star and its low-separation neighbor for stars with significant parallax differences (left panel) and high Poisson probability (right panel). The excess is defined as the difference between the observed G − J color and the expected G − J color based on the star’s BP − RP color (Equation (7); (G − J)0). The dashed red line is an exponential function fit to the expected G − J excess data.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Left panel: distribution of Poisson probabilities for a companion to be a chance alignment based on the average local stellar field density (Equations (2)–(3)) for the 200 pc stars with a close neighbor (blue bins) and the surrounding field stars within 1′ (orange bins). Right panel: Ratio of the number of field stars to 200 pc stars with a close neighbor with probability greater than x. The ratio has been normalized such that it is assumed that 100% of stars in the highest probability bin are field stars.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Relations between Gaia eDR3 and DR2 photometry for each Gaia photometric band. For each relation, a second degree polynomial has been fit iteratively by clipping 1.95σ of the sources from the fit for 50 iterations until converging on the solution shown (red-dashed line).
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Left panel: The number of candidate binaries (blue line) and likely contaminants (orange line) given some cut in contamination factor, L cut, of being a chance alignment (Equation (9)). Here, the candidates are all candidate binaries that have L < L cut, while the contaminants are the number of candidates greater than what is expected for a 200 pc sample of stars based on their sky distribution. Finally, the green line shows the resulting number of candidate binaries if high contamination regions (>10%) on the sky are excluded. The red dotted line shows the ideal value of L cut = 0.00193. Right panel: The contamination rate (solid lines) and completion rate (dashed lines) for all candidate binaries with L < L cut (blue lines) and candidate binaries with L < L cut in low contamination regions (<10%; green lines). The red dotted line shows the ideal value of L cut = 0.00193.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Corner plot for all 200 pc stars with a close Gaia neighbor shows the distributions in G magnitude of the primary (G), sine of the Galactic latitude (sin(b)), Galactic longitude (l), ∣ΔG∣, G − J excess ((G − J) − (G − J)0), angular separation (θ), and the ipd_frac_multi_peak value from Gaia (image parameters determination multiple fraction; M.F.). All 2D distributions are log-scaled to better show low signal details in the distributions. All 1D distributions show the number linearly scaled.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Selection of Gaia stars that result from querying stars in our 200 pc sample within 10° of (l, b) = 330°, − 4°). The left panel shows the observed distribution (black line) for pairs of stars with 0 < ∣ΔG∣ < 1, and the right panel for pairs with 6 < ∣ΔG∣ < 7. The red-dashed lines shows the fit to the distributions, where the left panel fits a line in the outer region (θ > 2.″5) and a line plus a power law in the inner region (0.″7 <θ < 2.″5), while the right panel just fits a line to the outer region.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Density distribution of ∣ΔG∣ as a function of angular separation for the candidate binaries with L < 0.00193 and not in a high contamination region. Overlayed is the 1σ scatter of ∣ΔG∣ values in bins of angular separation of width 0.″1 for candidate binaries with L < 0.00193, not in a high contamination region and not found in the El-Badry et al. (2021) catalog (red-dashed line), and all binaries in the El-Badry et al. (2021) catalog within 200 pc (solid white line). This demonstrates that a larger portion of the new pairs in our catalog have larger ∣ΔG∣ values than in the El-Badry et al. (2021) catalog.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Same as Figure 7 except only for pairs that have significant parallax differences or high Poisson probability of chance alignment, which mean that the companion is a background source.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Sky plots in Galactic coordinates for the expected distribution of binaries from our model based on the 200 pc sample (top left), all likely binaries (top right), contamination rate in likely binaries (bottom left), and likely binaries in regions where the contamination rate is <10% (bottom right). The full list of candidate binaries is given in Table 1.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Distributions of angular separation (top panel) and projected physical separation (bottom panel) for the candidate binaries with L < 0.00193 and not in a high contamination region, and that were not previously found in the El-Badry et al. (2021) catalog (blue histograms). All the binaries in the El-Badry et al. (2021) catalog within 200 pc are also shown for comparison (orange histograms). For the projected physical separation for the likely binaries, the parallax of the Gaia eDR3 200 pc source was used to calculate projected physical separation, as many of the companions do not have parallax measurements.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: H-R diagram for a subset of the candidate binaries with L < 0.00193 and not in high contamination regions, where primaries are shown in the left panel, and secondaries in the right panel. In both panels, the parallax of the primary is used to calculate the absolute magnitude. The black data points are for likely binary primaries with parallax error <5%, open blue squares are for likely binaries not identified by El-Badry et al. (2021) with s < 30 au and parallax error >5%, and red closed circles are for likely binaries not identified by El-Badry et al. (2021) with s < 30 au and parallax error <5%.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Same as Figure 7 except for the clean sample of likely binaries.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: Left panel: Number density of projected physical separation vs. distance for likely binaries with θ > 0.″776, ∣ΔG∣ < 2, and 5.5 < M  G  < 8.15. The red-dashed lines indicate the minimum (θ = 0.″4) and maximum (θ = 2.″5) angular separation limits imposed. Middle panel: Number density plot shown in the left panel where each column has been normalized by the volume probed by each bin. Additionally, each bin has been arbitrarily scaled by 100 for readability. Right panel: Distribution of projected physical separations (black histogram) for the sample in the left panel. This distribution has been calculated by taking the average in each row in the middle panel where 100 × N binary/N star > 0. The distribution was bootstrapped over 1000 iterations to produce the uncertainties shown as the black error bars. The distribution is fit with a log-normal function of the form: ﹩f(x)=A\ {e}^{\tfrac{-{\left({\mathrm{log}}_{10}(x)-\mu \right)}^{2}}{2{\sigma }^{2}}}﹩, where x = s, and s is the linear, projected physical separation in astral units. The posterior distribution for the model parameters is probed using emcee, and the resulting 16th, 50th, and 84th percentiles of the distributions are shown in the legend of the figure.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. I. New Candidate Binaries within 200 pc of the Sun
Authors: Ilija Medan, Sébastien Lépine
Figure caption: The expected fraction of stars detected as a function of angular separation for various bins of ∣ΔG∣ given the sample selection for this study (outline in Section 2).
Paper: Extended Habitability of Exoplanets Due to Subglacial Water
Authors: Amri Wandel
Figure caption: Boundaries of the Habitable Zone under various climate and atmospheric models as a function of radiative flux received from the host star, relative to Earth. Dashed lines represent the extended boundaries due to subglacial liquid water suggested in this work: blue for the inner HZ boundary (nightside ice evaporates due to heat transport, the percentage marks the global transport parameter f) and violet for the outer one (Martian polar lakes). Solid green lines and green shading denote the conservative HZ boundaries: inner one (moist greenhouse) and outer one (maximum CO2 greenhouse), calculated using the 1-D climate model. Also marked is the recent Venus boundary (dashed green line). The orange curve marks the tidal locking radius. Circles denote the terrestrial planets in the solar system and a few Earth-sized exoplanets orbiting M-dwarf stars.
Paper: Extended Habitability of Exoplanets Due to Subglacial Water
Authors: Amri Wandel
Figure caption: Maximal (red) and minimal (blue) boundaries of the atmospheric heating factor vs. instellation, for three values of the heat transport parameter: f = 0.2 (solid), 0.5 (dashed), and 1 (dotted). GJ 468 b and a few representative planets from Figure 1 are marked as green vertical bars, with the width showing the uncertainty in the instellation.
Paper: An Investigation of New Brown Dwarf Spectral Binary Candidates From the Backyard Worlds: Planet 9 Citizen Science Initiative
Authors: Alexia Bravo, Adam C. Schneider, Daniella Bardalez Gagliuffi, Adam J. Burgasser, Aaron M. Meisner, J. Davy Kirkpatrick, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Arttu Sainio, Les Hamlet
Figure caption: Observed SOAR/TripleSpec4.1 spectra for W0727−3607 (top), W1036−5144 (middle), and W1344−7320 (bottom), with gray lines showing the full resolution and black lines showing the spectra smoothed to the resolution of the standards and binary templates (R ≈ 150) according to their parallax-based absolute fluxes. The left-hand column depicts the best-fitting single standards (orange line) for the spectra of the three candidates while the right-hand column shows both the binary template (orange line) and the standard spectra that compose it (purple line for primary, blue line for secondary). Reduced ﹩{\chi }_{\nu }^{2}﹩ values are reported for each of the fits.
Paper: An Investigation of New Brown Dwarf Spectral Binary Candidates From the Backyard Worlds: Planet 9 Citizen Science Initiative
Authors: Alexia Bravo, Adam C. Schneider, Daniella Bardalez Gagliuffi, Adam J. Burgasser, Aaron M. Meisner, J. Davy Kirkpatrick, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Arttu Sainio, Les Hamlet
Figure caption: Index-index plots highlighting regions defined in Burgasser et al. (2010) and Bardalez Gagliuffi et al. (2015), as indicative of spectral binarity (red-shaded regions). Background gray points are SPLAT objects with spectral types between L3 and T8. The three targets of this study are shown in the legend.
Paper: An Investigation of New Brown Dwarf Spectral Binary Candidates From the Backyard Worlds: Planet 9 Citizen Science Initiative
Authors: Alexia Bravo, Adam C. Schneider, Daniella Bardalez Gagliuffi, Adam J. Burgasser, Aaron M. Meisner, J. Davy Kirkpatrick, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Arttu Sainio, Les Hamlet
Figure caption: Index-index plots highlighting the regions indicative of photometric variability defined in Ashraf et al. (2022; green-shaded regions). Background gray points are SPLAT objects with spectral types between L7 and T3, with our three observed targets indicated shown in the legend.
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Example of an ﹩i^{\prime} ﹩ light curve being fit with a template. Top: The raw light curve for star 2636 compared with the envelope of light curves of other stars in the field normalized to the same brightness and S/N. Middle: The same light curve passed through a high-pass filter, corrected with the mean offset of the other normalized light curves with error bars set by the spread of those light curves. Bottom: The goodness of fit of an occultation template sliding along the light curve, as measured by the Mahalanobis distance between the observed light curve and template at each point based on the autocorrelation measured from the light curve. The 1σ and 2σ ranges of the template distance expected from simulated, injected occultation events are indicated here. An inset of the labeled occultation-like signature in this light curve alongside the associated template is shown in the upper row of Figure 7.
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: The 95% confidence upper limits for the ecliptic sky density of kilometer-scale KBOs larger than the plotted diameters, compared with earlier limits set by TAOS (Zhang et al. 2013) and W-FAST (Nir et al. 2023), as well as the claimed detections from HST/FGS (Schlichting et al. 2012), CoRoT (Liu et al. 2015), and OASES (Arimatsu et al. 2019). The labeled distances indicate the approximate range of KBO distances covered by each survey/upper limit curve.
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Comparison of the estimated number of included stars vs. fraction of included occultations for a range of false negative fraction thresholds β, showing an optimum in relative sensitivity (the product of the two quantities) near the chosen ∼15.9% (i.e., 1σ level of the normal distribution).
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Demonstration of simulated frame matching, showing the red channel (﹩i^{\prime} ﹩) frame in Figure 1 (left), the simulated model frame (center), and the observed minus simulated residual frame (right), with the residuals (on the order of only ∼0.1% of the peak flux) amplified by 100× for visibility. It should be noted that the observed frame has been shifted into alignment with the simulated frame centered on the field of the nightly reference frame, from which the true camera pointing slightly drifts over the course of each night.
Paper: CHIMERA Occultation Constraints on the Abundance of Kilometer-scale Kuiper Belt Objects
Authors: Qicheng Zhang, Gregg W. Hallinan, Navtej S. Saini, Hilke E. Schlichting, Leon K. Harding, Jennifer W. Milburn
Figure caption: Example of nearly simultaneous 30.39 ms exposure frames of M22 through the blue (﹩g^{\prime} ;﹩ left) and red (﹩i^{\prime} ;﹩ right) channels after bias and flat calibration. The ﹩g^{\prime} ﹩/﹩i^{\prime} ﹩ images in this and subsequent figures are tinted blue/red for clarity.