adsabs/AstroCLIMB huggingface dataset:
Paper: Technosignature Searches with Real-time Alert Brokers
Authors: Eleanor M. Gallay, James R. A. Davenport, Steve Croft
Figure caption: Transit zone angle geometry. The yellow and blue circles represent the Sun and planet, respectively (sizes not drawn to scale). R⊙ is the solar radius and Rp is the planet’s radius. The average distance between the planet and the Sun is r (1 au for Earth), and ϕTZ is the full transit zone angle. The transit zone is a projection of ϕTZ onto the sky. Any theoretical sensor in this strip of sky could detect the planet’s existence via the transit method. Using similarity reasoning, we calculate ϕTZ =.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Histogram for the differences in rovibrational CO and the H I Pfund β (Pfβ) emission detection rates separated by stellar subtype: TTS (left) and Herbigs (right). The percentage on top of each bar is relative to the total number of the stellar subtype.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: the collected sample from C. F. Manara et al. (2023) with decl. plotted vs. stellar mass; up-side triangles represent objects with only an upper limit on the associated dust mass. Objects that are also within our sample are plotted with orange diamonds if we detected CO and green squares if no CO was detected. The vertical dashed line represents a stellar mass of 0.3 M⊙, and the horizontal dashed line represents a decl. of −40. Right panel: the same sample as the left figure, but only for sources with decl. > −40, which presents dust mass as a function of stellar mass. The lighter-gray circles represent objects at the edge of Keck’s observation limit (−35° to –40° decl.).
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Histograms of the rovibrational CO emission detection rate in our sample as divided by (top left) SED classification, (top right) stellar subclass, (bottom left) TTS subtype, and (bottom right) Herbig Meeus group. The taller, empty bar represents the total number of each subtype within our sample, while the filled-in portion of the bar represents the portion of the subtype with rovibrational CO emission detected. Percentages marked note the percentage of CO detections for each grouping.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Keck-NIRSPEC spectra that serve as examples as the five major types of rovibrational CO emission seen from Class II objects: strong CO CTTS (DR Tau), transition disk CTTS (DoAr 44), strong CO Herbig Ae/Be (AB Aur), weak CO Herbig Ae/Be (MWC 614), and transition disk Herbig Ae/Be (HD 141569). The location of all CO lines in the wavelength range are marked with a dashed gray line. In both of the strong CO examples, the 13CO and CO (2–1) transitions are also visible.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Three example Keck-NIRSPEC spectra of the different stellar classes of pre-main-sequence (PMS) objects: Class I (blue, LDN 1489), II (purple, DR Tau), and III (green, DI Tau). These spectra include two of the echelle orders from the “M-wide” filter. The dashed gray lines represent rovibrational CO(1–0) line wavelengths from HITRAN (I. E. Gordon et al. 2022), and the shaded pink region represents the location of the H I Pfund β transition. The additional emission/absorption lines visible adjacent to the marked CO(1–0) transitions are from CO(2–1) and 13CO(1–0) transitions.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Histogram of the total number of objects in each spectral class color-coded by which star-forming region or group they are associated with. The majority of our targets come from Taurus or Ophiuchus. The “Other” classification includes regions or groups with only a handful of stars that meet our detection criteria, or objects with no known, or conflicting, region membership in the literature.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: experimental radius vs. stellar luminosity. The gray shaded region represents a range of excitation temperature radii cutoffs, calculated from the stellar luminosity: the larger outer radii are for 250 K, and the smaller outer radii for a temperature of 1500 K. Right panel: retrieved emitting area vs. stellar luminosity. Poor retrievals are marked with the plus sign, as defined in Section 4.3.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Generated slab models of rovibrational CO in a disk with different temperatures and column densities. In the left panel, temperature is held constant (at 1200 K), while only column density is varied from 1016.25 to 1018.75 cm−2 with steps of 0.25 in log space. The lower rotation curves (purple) represent lower column density, representing optically thin disks, while the higher rotation diagram curves (yellow) have higher column densities and illustrate how optical thickness effects the shape of a rotation diagram. In the center and right panels, column density is held constant (at 1016 cm−2 and 1018 cm−2, respectively) while temperature is varied from 500–1500 K with steps of 100 K. Lower temperatures (purples), have steeper slopes, while higher temperatures (yellows) are flatter.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: retrieved temperature vs. RCO. Middle panel: retrieved temperature vs. Rret. Right panel: retrieved temperature vs. experimental outer radius, Rout. The dashed lines are the surface dust temperatures for large and small grains calculated via the prescriptions from C. P. Dullemond et al. (2001). Poor retrievals are marked with the plus sign, as defined in Section 4.3.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: the CO luminosity vs. the stellar accretion rates (Table 1). Object subclasses are marked by the symbols denoted in the top-left corner. The gray dashed line is the linear fit for the full sample in log–log space. Right panel: the CO luminosity vs. the stellar mass (Table 1). Object symbols are the same as the left panel.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Example rotation diagrams for the six objects presented in Figure 5: strong CO CTTS (DR Tau), hot CO TTS (CI Tau), transition disk TTS (DoAr 44), strong CO Herbig Ae/Be (AB Aur), weak CO Herbig Ae/Be (HD 179218), and transition disk Herbig Ae/Be (HD 141569). The data are plotted in blue circles, and a slab model rotation diagram generated from our best-fit parameters is plotted as a green dashed line.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Histograms for the retrieved properties for the entire sample separated by disk subtype: TTS (purple, right hatch, dashed line), Herbig (green, left hatch, dashed–dotted line), and transition (blue, vertical hatch, dotted line). From left to right, the retrieved properties are column density, emitting area, and temperature. The vertical lines are representative of the medians for each subsample, colored to match their respective subtype.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: the average CO emission-line width vs. stellar luminosity with the stellar subtypes marked as in legend. Right panel: the same CO line width vs. millimeter-dust disk inclination. The gray shaded region represents the range of predicted broadening due to Keplerian rotation at the sublimation radius around a K7 TTS to an A5 Herbig.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: The P(10) CO line-to-continuum ratio vs. the CO luminosity (left) and the accretion rate (right).
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: the retrieved column densities vs. the accretion rate for all sources with retrievals and accretion rates. The stellar and disk subtypes are as marked in the legend. Right panel: the retrieved temperatures vs. the accretion rate for the sample. Poor retrievals are marked with the plus sign, as defined in Section 4.3.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: The deprojected retrieved emitting area plotted against RCO, the Keplerian radius at HWHM. The purple triangles are CTTSs, the green squares are Herbigs, and the blue circles are transition disks, while objects with poor retrievals (as defined in Section 4.3) are marked with a plus symbol. The different dashed lines correspond to A = 2πRΔR: ΔR = 10 is dotted, ΔR = 0.5 is dashed, and ΔR = 0.01 is dotted–dashed. The solid black lines correspond to a circle, A = 2πR2.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: The three different explanations for physical processes that could be causing the observed emitting area of the CO. In all three, the disk is represented in orange while the red, striped region represents the CO emitting area. (a) The emitting area is determined by the temperature of the CO. (b) The emitting area is determined by structure in the disk—in this cartoon, by a planet-caused ring. (c) The emitting area is always a thin ring of width ΔR.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Left panel: integration time to reach a 3σ detection of the P(10) CO rovibrational emission line vs. the continuum flux of the object at 4.75 μm. The shaded region correspond to a range of LTC ratios (0.22–0.50 for Keck, and 0.11–0.25 for JWST), representative of average values from our sample. The intersection of Keck and JWST is represented by a gray line at 0.3 Jy. Right panel: same as the left panel, but for the P(30) CO rovibrational emission line and JWST-MIRI-MRS and the continuum flux at 4.95 μm. The range of LTC ratios represented for the P(30) line are 0.09–0.39 for Keck, and 0.05–0.20 for JWST. The intersection line is at 1.03 Jy.
Paper: A Comprehensive Analysis of Rovibrational CO in the Era of JWST
Authors: D. Annie Dickson-Vandervelde, Colette Salyk, Geoffrey A. Blake, Clara Ross, Adwin Boogert, Klaus Pontoppidan
Figure caption: Rotation diagram for combined Keck-NIRPSEC and JWST-MIRI rovibrataional CO data for FZ Tau. Three slab models are shown on the graph based on three different data sets the retrieval was run on: just the Keck data (teal), just the JWST data (pink), and the combination of the two (black).
Paper: The James Webb Space Telescope Absolute Flux Calibration. IV. Near-Infrared Imager and Slitless Spectrograph Imaging
Authors: Kevin Volk, Paul Goudfrooij
Figure caption: The measured calibration factor values for the NIRISS F480M filter, including both imaging photometry observations and acquisition observations of photometric standards observed in other modes. The circles/diamonds/triangles give the individual measurements from the rate images. The squares represent the individual object mean values. The black diamond symbol is the result of averaging of the individual object mean values, while the red star symbol is the result of the inverse-variance weighting of the object mean values. The wavelengths on the x-axis are offset from the pivot wavelength by differing amounts to show the different points. The pivot wavelength is half-way between the wavelengths of the two overall mean values. The dashed line is the calibration factor derived during the commissioning of NIRISS.
Paper: The James Webb Space Telescope Absolute Flux Calibration. IV. Near-Infrared Imager and Slitless Spectrograph Imaging
Authors: Kevin Volk, Paul Goudfrooij
Figure caption: Example of the aperture used in the AMI mode imaging measurements: at left, displayed with an logarithmic scale to show the bad pixels, and at right, displayed on a linear scale. The solid red circle is the extraction aperture, and the outer dashed red circle is the outer limit of the background region. The image is in the F480M filter, which has the widest PSF of the NIRISS filters. Bad pixels have “not a number” (NaN) values in the images, which are masked to a value of 0.0 for the display. In this case, the lower four rows of pixels are reference pixels, which do not measure any light from the scene.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Ks-band image with a zoom-in of the W51A protocluster region showing the stellar density map. Dashed-line contours were created with 10″ × 10″ bins, and the solid black contours were created with 3″ × 3″ bins. The contour levels for both sets of contours start at 50% of the value of the most populated bin, increasing by 10% increments for each level. The lowest contour level (shown by the dotted contours) represents 134 stars pc−2 (0.08 stars arcsec−2), and the highest contour level (shown by the solid contours) represents 484 stars pc−2 (0.30 stars arcsec−2). The 1 mm Atacama Large Millimeter/submillimeter Array emission is shown by the blue contours. The defined protocluster regions are shown as the black polygons encompassing the areas of both high stellar density, and bright 1 mm emission. The solid line in the full FOV shows the region we have excluded due to poor image quality. Red X’s indicate the position of the extremely luminous sources discussed in Section 4.2.2.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: (a) H − Ks vs. Ks color–magnitude diagram of the region with 1 Myr isochrones reddened by AV = 0 and AV = 30 over-plotted. We specify the locations of 1, 5, and 10 M⊙ stars on the AV = 0 isochrone and the reddening line connecting to their locations on the AV = 30 isochrone. The estimated 90% completeness limit is shown as the segmented dashed–dotted line. (b) H − Ks vs. J − H color–color diagram of the region with an un-extincted, 1 Myr isochrone over-plotted in orange. The two solid, parallel lines encompassing the isochrone are the main-sequence (MS) reddening zone (reddening slope from G. H. Rieke & M. J. Lebofsky 1985; see Section 3.2.). The dashed line indicates the locus of classical T-Tauri stars (CTTS; M. R. Meyer et al. 1997), which is encompassed by the leftmost solid line and the dashed–dotted line, showing the boundaries of the CTTS locus reddening zone. The dotted line represents the Herbig AeBe star locus (C. J. Lada & F. C. Adams 1992).
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Background-subtracted Ks-band image showing newly detected sources in W51 IRS2 (left) and W51 Main (right). The magenta star markers show the location of stars that have had their spectral type/evolutionary stage estimated (see Appendix E).
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Histograms comparing the distribution of (a) apparent Ks-band magnitude and (b) extinction (﹩{A}_{{K}_{s}}﹩) between the newly discovered and previously documented stars in the W51A protoclusters (see Section 4.2).
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: The J, H, and Ks ePSFs used in the star-finding algorithm with an FWHM of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩13, 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩74, and 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩55, respectively. The pixel size in each figure is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩097.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Extinction contours over-plotted on the W51A protoclusters. Contour labels are given in visual extinction (AV). The contours were created with 10″ × 10″ bins, and smoothed using a 2D Gaussian kernel with an 8 pixel width.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Ks-band image focused on the central H II region of W51A. The red X’s show the location of sources with an H − Ks color greater than 2.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: Ks-band completeness curves for three regions in W51A: W51 IRS2, W51 Main, and the region south of the protoclusters with no diffuse emission.
Paper: How Massive Star Clusters Form and Evolve: A Near-IR Survey of the W51 Complex
Authors: Aden Dawson, Adam Ginsburg, Carlos G. Román-Zúñiga
Figure caption: RGB (KsHJ) image of W51A created from our observations.
Paper: Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System
Authors: Morgan Saidel, Shreyas Vissapragada, Michael Zhang, Heather A. Knutson, Matthäus Schulik, Jorge Fernández Fernández, Michelle Kunimoto, Peter J. Wheatley, Jessica Spake
Figure caption: Transiting planet radii, periods, and densities in the vicinity of the Neptune desert, drawn from the NASA Exoplanet Archive on 2025 April 4 (R. L. Akeson et al. 2013; NASA Exoplanet Archive 2024). The dashed lines indicate the Neptune desert, ridge, and savanna boundaries from A. Castro-González et al. (2024). Planets in the TOI-4010 system are indicated with a star and a darker opacity.
Paper: Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System
Authors: Morgan Saidel, Shreyas Vissapragada, Michael Zhang, Heather A. Knutson, Matthäus Schulik, Jorge Fernández Fernández, Michelle Kunimoto, Peter J. Wheatley, Jessica Spake
Figure caption: In-transit spectra of TOI-4010 b (first panel), TOI-4010 c (second panel), and TOI-4010 d (third panel) in the stellar rest frame. Gray lines are the in-transit spectra throughout the night. The average in-transit spectrum is shown in black. Red vertical dashed lines denote the wavelengths of the three helium lines. The red shaded regions correspond to the location of a telluric OH line and are masked in our analysis.
Paper: Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System
Authors: Morgan Saidel, Shreyas Vissapragada, Michael Zhang, Heather A. Knutson, Matthäus Schulik, Jorge Fernández Fernández, Michelle Kunimoto, Peter J. Wheatley, Jessica Spake
Figure caption: Top row: Keck/NIRSPEC excess absorption in percent of TOI-4010 b (first panel), TOI-4010 c (second panel), and TOI-4010 d (third panel) in each planet’s rest frame as a function of time and wavelength (air wavelengths in planetary rest frame). Horizontal white lines mark the beginning (top) and end (bottom) of transit. Dashed vertical red lines denote the positions of the three helium lines. Red shaded regions mark the location of a telluric OH line that we masked in our analysis (see Figure 2). Bottom row: average excess absorption spectra for TOI-4010 b (first panel), TOI-4010 c (second panel), and TOI-4010 d (third panel) are shown as black points. The pyTPCI solar metallicity model predictions of the excess absorptions are shown as a blue line (nominal XUV flux), purple line (XUV flux reduced by a factor of five), pink line (XUV flux reduced by a factor of 10), and orange line (XUV flux reduced by a factor of 15).
Paper: Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System
Authors: Morgan Saidel, Shreyas Vissapragada, Michael Zhang, Heather A. Knutson, Matthäus Schulik, Jorge Fernández Fernández, Michelle Kunimoto, Peter J. Wheatley, Jessica Spake
Figure caption: Top row: posterior probability distribution for log ﹩\dot{M}﹩ and T0 for TOI-4010 b (first panel), TOI-4010 c (second panel), and TOI-4010 d (third panel). The contours indicate the 1σ, 2σ, and 3σ levels for the distributions. The pyTPCI solar metallicity-predicted mass loss rates and estimated outflow temperatures are shown as blue circles (nominal XUV flux of stellar spectrum), purple circles (XUV flux reduced by a factor of five), pink circles (XUV flux reduced by a factor of ten), and orange circles (XUV flux reduced by a factor of 15). Bottom row: p-winds predicted excess absorptions corresponding to our MCMC analysis for a 50 × 50 grid sampling our ﹩\dot{M}﹩–T0 prior range.
Paper: Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System
Authors: Morgan Saidel, Shreyas Vissapragada, Michael Zhang, Heather A. Knutson, Matthäus Schulik, Jorge Fernández Fernández, Michelle Kunimoto, Peter J. Wheatley, Jessica Spake
Figure caption: Left panel: evolution of the radius of TOI-4010 b under atmospheric escape and thermal contraction, as described in Section 5.5. The solid lines show evolution under different starting envelope mass fractions of 1%, 2%, and 5%, and the shaded regions represent the uncertainties on each evaporation history, given the uncertainties in the planet’s parameters and the XUV emission history of its host star. The planet’s present-day age and radius are plotted as a red circle. Right panel: evolution of the envelope mass fraction of the gaseous atmosphere of TOI-4010 b, following the left panel.