adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: Posterior distributions of the seven classical orbital elements plus the (fitted) orbital parallax, the Gaia DR2 trigonometric parallax and its ±1σ error, the systemic velocity, the velocity amplitudes for both components, the mass sum, the mass ratio, and the individual component masses for the same objects shown in Figure 2. We note that for objects with a mass ratio close to 1 (in this case, A2983, middle panel; but see Table 4 for other objects), the mB/mA histograms are well behaved and smooth across that boundary, as explained in the text.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: Comparison of trigonometric and orbital parallaxes for our sample of SB2s. The left panel shows a comparison of our orbital parallax ΠOrb with the Hipparcos parallax (from the rereduction by van Leeuwen 2010), the Gaia eDR3 parallax, and the orbital parallaxes from Piccotti et al. (2020). The correlation is good and tight. The dotted–dashed line is a one-to-one relationship shown for reference. In the right panel, we plot the deviation of ﹩\left({{\rm{\Pi }}}_{{\rm{Orb}}}-{{\rm{\Pi }}}_{{\rm{Various}}}\right)/{\sigma }_{{\rm{\Pi }}}﹩, where σΠ includes our uncertainty and those quoted for Hipparcos, Gaia, and Piccotti in Table 4. The four most discrepant cases, identified in the plot, are discussed further in Section 5.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: The H-R diagram for our sample of SB2 systems with available photometry. Green dots depict primary components, and orange dots depict the secondaries. Each pair has been linked with a line, and the discoverer designation is noted. The bar at (0.6, 8.0) shows the estimated error of the photometry, as discussed in Section 2. For reference, we have plotted an empirical ZAMS, three solar-metallicity (Z⊙ = 0.0152) 5 Gyr old theoretical isochrones, and a 9 Gyr isochrone. In the inserted table, we show a comparison of our estimated masses and the mass predicted by the theoretical models. See text for details and comments on individual systems.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: Same as Figure 5 but for objects with dubious photometry. Having corrected their photometry using the procedure explained in the text, we depict their putative location on the H-R diagram. The table inserted in the figure gives their measured and “corrected” photometry.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: The ML orbit for TOK39Aa,Ab. Symbols are the same as in Figure 2. Shown is the solution without a prior. As explained in the text, if a parallax prior is used, the resulting plot is quite similar. The currently incomplete orbital coverage justifies the use of a high-precision Gaia parallax prior, which significantly improved the precision of our estimate of the individual component masses (see Figure 8).
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: Posterior distribution functions for TOK39Aa,Ab. The top panel shows the solutions obtained without a parallax prior, and the bottom panel shows those obtained with a parallax prior. Note that in the top panel, the mass scale is logarithmic, while in the bottom panel, it is linear. Even in the no-prior scenario, the interquartile range and ML value for the parallax are commensurate with the Gaia eDR3 value.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: The code structure of ThERESA. The blue boxes show the inputs or stages of the analysis, with arrows showing the order of execution. The background colors show which code(s) perform each stage. The steps within the MC3 boxes are run thousands of times by MC3, but the calculations are handled by ThERESA (unless otherwise noted).
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Top left: the positive and negative spherical-harmonic maps with l ≤ 2, omitting the uniform map ﹩{Y}_{0}^{0}﹩. Bottom left: the secondary-eclipse light curves from integrating the spherical-harmonic maps in the top left. Light-curve colors match the corresponding maps. Dashed lines correspond to negated spherical-harmonic maps. Bottom right: the eigencurves with the eight largest eigenvalues resulting from truncated singular-value decomposition principal component analysis applied to the spherical-harmonic curves in the bottom left. Eigenmaps are ordered, left to right, from most to least information content. Top right: the eigenmaps corresponding to each eigencurve in the bottom right, with matching colors.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Results of a 2D fit to the HD 189733 b Spitzer observations. Top: the light-curve data and best-fitting model. The inset shows the best-fitting thermal map. A black box covers the longitudes not visible during the observations. The hot-spot location is marked with a black dot. Bottom: the model residuals and uncertainties. Data are binned for visual clarity, to 10 data points per bin.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: The temperature grid used in light-curve generation. The colored profiles show temperatures at various longitudes along the equator. The substellar point is 0°. All other thermal profiles are plotted in gray.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Uniform-map and eigenmap components of the 2D fit to the 2.05 μm light curve. The magnitude of each map has been scaled by the best-fitting ci value. The vertical dashed lines denote the minimum and maximum visible longitudes during the observation, at −126° and 126°.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: 2D fits to each of the spectroscopic light curves and the residuals.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Comparison between input thermal maps and retrieved 2D maps. Dashed lines indicate the edges of the visible portion of the planet. The GCM hot-spot location (see main text) is marked with a star and the fitted hot-spot location is marked with a diamond. Left: thermal maps from the GCM, computed using filter-integrated flux maps and Equation (3). Right: 2D thermal maps derived from fits to each light curve. The maps are plotted at the resolution of the GCM, but these maps can be computed at an arbitrary resolution. The blank spaces have undefined temperatures, as the 2D fit produces negative flux in those regions. This is permitted because those grid cells are never visible during the observation, so we formally have no information about them.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Top: the normalized ingress of a uniformly bright WASP-76b, computed by integrating the planet with the visibility function (Equation (7)) for a range of grid sizes, compared to the true ingress shape computed analytically with starry. Bottom: the difference between the true ingress and the gridded planets. The dashed lines indicate the normalized 1σ region for the highest signal-to-noise filter in our synthetic observation of WASP-76b. The light curve of a sufficiently high-resolution grid should fall within these boundaries.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Left to right: the input temperature grid from the GCM, the isobaric retrieval, the fixed-phase sinusoidal retrieval, the free-phase sinusoidal retrieval, and the quadratic retrieval. The colored lines indicate temperature profiles along the equator, with the GCM downsampled to the spatial resolution of the fitted temperature grid. All others are plotted in gray. For the fitted grid, the plotted color opacity for each profile is weighted by the maximum contribution function (over all filters) for each grid cell and pressure layer, normalized to the largest contribution. Nonvisible grid cells have a contribution of 0. Dots indicate the placement of the 2D temperature maps for each (visible) grid cell, and their plotting opacity is the ratio of the total contribution from that grid cell and filter to the maximum total contribution.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Histograms of hot-spot longitude from the MCMC posterior distributions for each 2D map. The best-fitting hot-spot longitude is overplotted in a red line. The GCM hot-spot longitude is shown with a black line if it falls within the longitudes of the x-axes.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Uncertainties in the 2D temperature map fits, calculated as the standard deviation of the posterior distribution of maps. Plots are at the spatial resolution of the GCM, although they can be computed at any resolution. Axes are limited to locations visible during the observation. Left: difference between the GCM (in black) and fitted equatorial temperatures. The shaded regions denote the 1σ, 2σ, and 3σ boundaries. Right: temperature uncertainty maps, calculated as the standard deviation at each location.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: A comparison of the equatorial temperature uncertainties on 1.14 μm maps retrieved with different numbers of eigencurves. The blue region denotes 1σ, 2,σ and 3σ. Only visible longitudes are shown. Top: the equatorial temperatures of the GCM and the best fit. Middle: the difference between the GCM and fitted equatorial temperatures. The blue data point shows the best-fit hot-spot longitude and its 3σ uncertainty (y location arbitrary). Bottom: the fraction of the observation during which a given longitude, along the equator, is visible to any degree, including the effects of both planet rotation and the occultation by the star. The plateau centered on 0° shows the longitudes, which are visible for the whole observation, except during eclipse. The smaller plateaus near −90° and 90° are the longitudes visible for the entirety of pre- or posteclipse but not vice versa due to planet rotation during eclipse.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: MCMC posterior distribution of temperature profiles at the substellar point, showing our parameterization scheme is not influencing the location of the thermal inversion. For computational feasibility, we thinned the posterior distribution by a factor of 100. Top: the minor positive correlation between Tbot and the pressure at the top of the thermal inversion, where the temperature gradient becomes negative. Bottom: the distribution of temperature–pressure profiles in the MCMC posterior near the thermal inversion at the substellar point. At lower pressures the atmosphere is isothermal and at higher pressures, the linear trend continues down to Tbot at 100 bar.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: Left: the light-curve fit from the best-fitting 3D model, and the residuals. Right: contribution functions, normalized to the maximum contribution, for visible grid cells along the equator in the best-fitting 3D model. Each panel shows a different filter. The gray boxes indicate the range of pressures covered by the respective 2D map.
Paper: ThERESA: Three-dimensional Eclipse Mapping with Application to Synthetic JWST Data
Authors: Ryan C. Challener, and Emily Rauscher
Figure caption: The normalized equatorial contribution functions for each spectroscopic bin. The vertical, equatorial placements of the 2D thermal maps from the optimal fit of the free-phase sinusoidal function (Table 4) are overplotted in red.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: These histograms show the distribution of the initial (blue) and final (green) moving object training sets across W1 − W2, W2 and total proper motion. Note that for our W1 − W2 histogram we only plot objects that had W1 − W2 values between −0.5 and 4.0 mag.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: J − W2 vs. J-Ks color–color diagram. The orange points are discoveries announced in this paper. For comparison, other proper motion discoveries from Figure 7 of Kirkpatrick et al. (2016) are plotted as blue points. The green arrows denote color limits. Objects labeled in purple are discussed in the text. Note that the UHS discoveries are not plotted on this diagram because they have no Ks data.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: W1 − W2 vs. J − W2 color–color diagram. The orange points are discoveries announced in this paper. For comparison, other proper motion discoveries from Figure 8 of Kirkpatrick et al. (2016) are plotted as blue points. The green arrows denote color limits. Objects labeled in purple are discussed in the text.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: Time-series photometry of CWISE J235713.17−630827.3. The first row illustrates the entire light curve in three different sectors. The second row illustrates the periodogram for each of the light curves above.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: Finder charts for CWISE J2158−0854 and CWISE J2357−6308. The finder chart shows a >30 yr baseline of time. DSS2 R, 2MASS J, WISE W1, and WISE W2 images are shown. The objects have small but clear proper motions. Each cutout is 2′ on a side, with north up and east to the left.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: Finder charts for CWISE J1230+3801 and CWISE J1848−8757. The finder charts illustrate the faintness of the objects. The UHS J, WISE W1, and WISE W2 images are shown for CWISE J1230+3801. The VHS J, WISE W1, and WISE W2 images are shown for CWISE J1848-8757. Each cutout is 2′ on a side, with north up and east to the left.
Paper: Discovery of 16 New Members of the Solar Neighborhood Using Proper Motions from CatWISE2020
Authors: Tarun Kota, J. Davy Kirkpatrick, Dan Caselden, Federico Marocco, Adam C. Schneider, Jonathan Gagné, Jacqueline K. Faherty, Aaron M. Meisner, Marc J. Kuchner, Sarah Casewell, Kanishk Kacholia, Tom Bickle, Paul Beaulieu, Guillaume Colin, Leslie K. Hamlet, Jörg Schümann, and Christopher Tanner
Figure caption: Finder charts for CWISE J0400−5111 and CWISE J1840+4107. For CWISE J0400-5111 these are three-color images made from DES g, i, and y, VHS J, H, and Ks, and WISE W1, W2, and W3. For WISE J1840+4107, the images are PSO g, i, and y, UHS J, and WISE W1, W2, and W3. (Only one band was available for UHS.) For CWISE J0400-5111, the red color in the optical (DES), the blue color in the near-infrared (VHS), and the green color in the mid-infrared (WISE) parallel the spectral energy distribution of a T dwarf. CWISE J1840+4107 has less information than CWISE J0400−5111, but is faint in the optical, detected at J, and brighter and green in the WISE bands, again characteristic of a T dwarf.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: 1999 Keck/LRIS R-band image (﹩\sim 6^{\prime} \times 8^{\prime} ﹩) with orientation north upwards and east to the left. Bright nebulosity is associated with both BD+40° 4124 (center) and V1686 Cyg (southeast of center). The LkHα 225 North–South pair are due east of V1686 Cyg. At this epoch, LkHα 225 South (indicated by red arrow) was in a prolonged faint state (see Figure 3).
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Top panel: expanded view of the faint-state 1999 Rc-band image of Figure 1, centered here on the LkHα 225 system, with LkHα 225 North and LkHα 225 South both marked. The well-known ridge of nebulosity between them is faint in this stretch, but can be seen extending from North southward to a nebular knot. An even brighter nebular knot along the same line, about 0.8″ northeast (PA = 35.5°) of LkHα 225 South, is marked. The position appears to be coincident with maser spots and 3.1 mm continuum emission; see text. The knot is brighter than LkHα 225 South itself at this particular epoch, and it has some east–west extension. At the western edge of the image, the extended bright nebulosity is associated with V1686 Cyg (LkHα 224) which is just off frame. Bottom panel: bright-state Y-band image taken in 2020 with Keck/NIRSPEC-SCAM; white pixels indicate saturation in the individual 0.655 sec exposures. The frame stack comprises 30 seconds of total integration. Relative to the earlier image above, LkHα 225 South has brightened dramatically compared to LkHα 225 North. A faint instrumental ghost appears to the northeast of LkHα 225 South; this is not the same position as the nebular source marked in the top panel.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Light curve for LkHα 225 South from the 1980s to the present, demonstrating the gradual fade over about 15 yr and subsequent rise by >6 mag over the next 20 yr. The published R-band data have been transformed to r using an advertised transformation equation (http://www.sdss3.org/dr8/algorithms/sdssUBVRITransform.php#Lupton2005), with the correction here typically a shift by 0.6 mag fainter. The PanSTARRS and ZTF photometry has been converted from native AB to Vega magnitudes. The Gaia DR2 G-band photometry has been corrected into the r band using the transformation equation derived by Hillenbrand et al. (2018), in this case around 0.1 mag fainter. Data points from Herbst & Shevchenko (1999) are lower limits and based on their measured V-band brightness and an assumed V − R > 3 mag, then using the above conversion to r. Expansion of part of the ZTF time series appears in Figure 4.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: LkHα 225 South time series obtained in the r band and g band by the ZTF in the 2018 and 2019 seasons; error bars are plotted but are generally smaller than the points. The source is clearly quasiperiodic in the outburst state, with an oscillation timescale of a little more than a month. The g-band photometry reported by ASAS is also included. The ∼1 mag offset between the ASAS and ZTF g-band measurements is likely a result of the large ASAS pixels; added variability from LkHα 225 North on top of the quasiperiodic variations exhibited by LkHα 225 South perhaps explains the inconsistencies, e.g., around MJD ≈ 8350 and 8390 days. Epochs of spectroscopy are indicated and labeled.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: LkHα 225 South low-dispersion optical spectrum from Palomar/DBSP (magenta) and infrared spectrum from IRTF/SpeX (red). LkHα 225 South appears significantly reddened, even in outburst. Figures 6 and 9, respectively, offer expanded views of the optical and infrared portions of the spectra. Inset illustrates the strong Na ID and Hα features; both have blueshifted absorption components when examined in higher spectral dispersion data (see Figure 11).