adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Decay in M82 X-2
Authors: Matteo Bachetti, Marianne Heida, Thomas Maccarone, Daniela Huppenkothen, Gian Luca Israel, Didier Barret, Murray Brightman, McKinley Brumback, Hannah P. Earnshaw, Karl Forster, Felix Fürst, Brian W. Grefenstette, Fiona A. Harrison, Amruta D. Jaodand, Kristin K. Madsen, Matthew Middleton, Sean N. Pike, Maura Pilia, Juri Poutanen, Daniel Stern, John A. Tomsick, Dominic J. Walton, Natalie Webb, Jörn Wilms
Figure caption: Left: orbital decay in M82 X-2, measured through the delay of the T asc parameter (time of passage through the ascending node) from Equation (3). Semitransparent orange lines indicate possible ∼1000 quadratic solutions, coming from MCMC sampling (described in Section 3.1). Grey points are lower-quality measurements (uncertainty in T asc larger than 200 s due to high orbital-spin parameter correlation). Right: corner plot of the posterior distribution of the parameters of the orbital decay with Equation (4), sampled with MCMC. Vertical dashed lines show the 16%, 50%, and 84% percentiles.
Paper: Orbital Decay in M82 X-2
Authors: Matteo Bachetti, Marianne Heida, Thomas Maccarone, Daniela Huppenkothen, Gian Luca Israel, Didier Barret, Murray Brightman, McKinley Brumback, Hannah P. Earnshaw, Karl Forster, Felix Fürst, Brian W. Grefenstette, Fiona A. Harrison, Amruta D. Jaodand, Kristin K. Madsen, Matthew Middleton, Sean N. Pike, Maura Pilia, Juri Poutanen, Daniel Stern, John A. Tomsick, Dominic J. Walton, Natalie Webb, Jörn Wilms
Figure caption: Pulsed amplitude vs. energy, using XMM-Newton data from ObsIDs 0870940101 and 0870940401, and NuSTAR data from ObsIDs 30602027002 and 30602027004. We overplot the raw count spectra of NuSTAR and XMM, showing how XMM-Newton has many more counts, but in energy intervals with little or no pulsations.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: 2D probability distribution function of N H I of the Gaussians in the σ–μ plane. Vertical gray line at μ = −10 km s−1 shows the boundary separating the BVC and LVC. Vertical black line at μ = 25 km s−1 represents the outer limit on the LVC range. Horizontal lines at σ = 2.3 km s−1 (red) and 5.4 km s−1 (blue) represent the CNM/LNM and LNM/WNM boundaries (see Section 4). Black points within the clusters represent the column-density-weighted means of each Gaussian cluster, tabulated in Table 1.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Column density and mass fraction maps (first and third column) with their associated standard deviation maps (second and fourth column) of the thermal phases in the NCPL, obtained using the means and standard deviations of the three methods described in Section 4.2.2. Rows from top to bottom show the CNM, LNM, WNMA, and WNMD, respectively. White points in the first column represent the position of the DF absorption source from the DHIGLS survey. Cyan and yellow lines represent contours of the total LVC column density, with levels of 1 × 1020  and 2 × 1020  cm−2, respectively.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: The upper panel is an example of the Gaussian decomposition obtained by ROHSA for the spectrum corresponding to the position annotated by the red point in Figure 4. Original signal is shown in gray and the total brightness temperature encoded by ROHSA is shown in black. Colored lines represent the individual Gaussian components. Red represents CNM, green represents LNM, and blue represents WNM. The lower panel shows the residual spectrum.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Gaussian decomposition of the averaged emission spectrum taken in a ∼2′ annulus centered on the source. The original signal is shown in gray and the total signal encoded by the Gaussians in black. The three individual Gaussians (solid lines) are color coded by phase, same as Figure 6. Gaussian decomposition by ROHSA from interpolation of the parameter maps in the same annulus is shown with dashed lines and the same color code. Parameters of the narrowest Gaussians are tabulated in Table 3.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Map of the reduced χ 2 obtained with ROHSA on the NCPL. The location of the spectral decomposition shown in Figure 6 is annotated by the red point.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: 2D distribution functions, showing how the various phase mass fractions are related to one another. Left column shows the relationship between LNM (top), WNMA (middle), and WNMD (bottom) and the CNM. First two rows of the right column show the relationship between the WNM components (WNMA: top, WNMD: middle) and the LNM. Bottom right panel shows the relationship between the two WNM components.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Column density maps of the thermal phases in the LVC, plus maps of the total BVC and IVC, in the NCPL. From left to right, the maps represent the CNM, LNM, WNMA, WNMD (all of the LVC), BVC, and IVC. Maps have the same dynamical range (color bar) to highlight the dominance of the CNM.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Three-phase view of the NCPL from column density maps of CNM (red), LNM (green), and WNMD+WNMA (blue). Maps were scaled with natural weightings to highlight their interrelationship and relative column densities.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Spectrum of mean contribution to chi-square for Gaussian models fit with different number of Gaussians. Horizontal line indicates 〈χ 2〉 = 1.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): time series of the T  B  of the impulsive events for various regions in Figure 9. The gray shaded region marks the times of quasi-periodic bursts mentioned in Section 6. The arrow in region 3 shows the drift burst location in time. Panel (B): 2D histogram of the number of impulsive emission for all the regions in frequency and duration. Panel (C): the top panel shows the zoomed-in time series of quasi-periodic bursts at 240 MHz; the bottom panel shows the drift burst in region 3.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): time-averaged T  B  of the 6σ and above bursts. Panel (B): the contours of the maps of T  B  of the 6σ and above bursts overlaid on the AIA 193 Å image. The contours plotted are 0.1, 0.5, and 0.9 times with regard to the map’s maximum. The green contour in each panel marks the 5σ map boundary of the radio solar maps, where σ map is the rms in the off-Sun region of the radio map. The black circle shows the optical disk position in each panel. Note that all color bars are logarithmic.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): a map of the total number of detected bursts at each of the frequency bands. Panel (B): 1σ temporal variation map of the 6σ and above features. The green contour in each panel marks the 5σ map boundary of radio solar maps, where σ map is the rms in the off-Sun region of the radio map. The black circle shows the optical disk position in each panel. Note that all color bars are logarithmic.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: AIA 193 Å image overlaid with 240 MHz radio map with the location of the six interesting regions. The red contour shows the 5σ map boundary of the 108 MHz radio maps, where σ map is the rms in the off-Sun region of the radio map. All regions are in within the solar radio disk.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): time-averaged residual T  B  maps for various frequency bands after removing 6σ and above time stamps. The white contour in each panel shows the 5σ map contour, where σ map is the rms computed in the off-solar-disk region in the residual solar maps. The green contour in each panel marks the 5σ map boundary of the radio solar maps. The black circle marks the edge of the solar optical disk. Panel (B): the contours of the time-averaged residual maps overlaid on the AIA 193 Å image. The contours are plotted at 0.6, 0.75, and 0.9 times the maximum.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panels (A) and (B) show histograms of the real and imaginary parts of the complex visibilities before and after continuum subtraction at 179 MHz. Panel (C) shows the visibility amplitude before and after the subtraction vs. baseline length for 179 MHz.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption:  T  B  distribution of all the reliably detected events at all frequencies along with a log–log fit. The yellow shaded region marks the T  B  range used to perform the power-law fit.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Examples of transient events seen in the residual solar maps. The black disk marks the size of the optical Sun. The contours indicate the boundary of the radio Sun by marking a level of 2 × 104 K. These maps come from the time range 03:24:36.5 to 03:24:37.0 UT.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption:  σ map  in the time-averaged image against the number of images averaged. The yellow line is proportional to ﹩1/\sqrt{N}﹩, where N is the number of averaged images.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Properties of the detected nonthermal bursts. Panel (A) shows the distribution of the area of the bursts relative to the beam area. Note that only 2.5% of events have an area greater than a PSF area. Panel (B) shows the distribution of the nonthermal particle energies for all the detected radio bursts. Note that the range between 1.5 × 1020–1021 erg marked as the yellow region was used for a linear fit in log–log space. Panel (C) shows the distribution of the radiated energy of the detected bursts.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): typical quiet Sun electron density (black), temperature (red), and magnetic field strength (green) model obtained from the PSIMAS model of 2015 December 3. Panel (B): For region 4 the plasma frequency as a function of coronal height obtained from the FORWARD model. The coronal height is measured from the solar surface. The gray shaded area shows the coronal height range corresponding to the type-III burst (Figure 10(C)).
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: In-painted column density map of the GHIGLS NCPL mosaic integrated over the spectral range −30.56 < v < 53.17 km s−1, calculated in the optically thin regime. Outside the black dashed contour are shown data from EBHIS over a similar velocity range (−29.52 < v < 51.63 km s−1). The solid white square shows the 256 × 256 pixel region on which our analysis is focused. White points represent the positions of the Ursa Major (UM; left) and DRAO Deep Field (DF; right) absorption sources from the DHIGLS survey.
Paper: Molecular Clouds as Gravitational Instabilities in Rotating Disks: A Modified Stability Criterion
Authors: Sharon E. Meidt
Figure caption: Growth rates for 2D Toomre instabilities (dashed lines) and for 3D instabilities at the midplane (solid lines) in a fully self-gravitating flattened disk (f  g  = 1; left) and a weakly self-gravitating flattened disk (f  g  = 0.5; right). The gray scaling of both sets of curves increases with increasing Q  T  (from 0 to 1). Curves with Q ≥ 1 are shown in red. As f  g  goes down, instabilities undergo faster growth on smaller scales at fixed Q  T , making 3D fragmentation more prominent than 2D structures in weakly self-gravitating disks.
Paper: Molecular Clouds as Gravitational Instabilities in Rotating Disks: A Modified Stability Criterion
Authors: Sharon E. Meidt
Figure caption: The behavior of ﹩{\mathscr{F}}﹩ (or ﹩1/(4\sqrt{2}{\gamma }_{T})﹩ in terms of γ  T  introduced in the text) that sets the threshold on ﹩\pi G\bar{\rho }/{\kappa }^{2}﹩ in the formalism of GLB and thus defines the onset of stability in 3D rotating flattened disks. The threshold calculated by GLB is shown in black. The approximation described in the text is shown as a black dashed line. Two gray horizontal lines depict the minimum threshold value calculated numerically in this work (﹩{\mathscr{F}}=0.56;﹩ dotted) and estimated by GLB (﹩{\mathscr{F}}=0.73;﹩ solid). Instability is possible whenever ﹩\pi G\bar{\rho }/{\kappa }^{2}\gt {\mathscr{F}}﹩ or whenever ﹩{\bar{Q}}_{M}\lt \sqrt{2}{\gamma }_{T}=1/(4{\mathscr{F}})﹩.
Paper: Molecular Clouds as Gravitational Instabilities in Rotating Disks: A Modified Stability Criterion
Authors: Sharon E. Meidt
Figure caption: Illustration of the behavior of F  z (x) (black) and F  r (x) (gray) as a function of x = h 1/h for finite wave perturbations in 3D flattened rotating disks. These functions appear in the 2D dispersion relation for finite vertical WKB perturbations with vertical extents ±h 1 and amplitudes that vary slowly as a function of height z from the midplane (1/z  p  < 1/z  d ); see Section 3.4. This example adopts the functional forms for F  z (x) and F  r (x) given by Equations (74) and (75), determined in the case of a constant-amplitude perturbation. A third dashed gray reference lines shows 1/x.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The light curves of KIC 3440495 in S40 and S41 obtained by using SAP. Top three panels: the time-series flux variation of the target with background, the time-series flux variation of the background, and the time-series flux variation after subtracting the background in S40 from left to right. Bottom three panels: the same for S41.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Mean H I spectrum of the region within the GHIGLS NCPL mosaic analyzed (the white box in Figure 2), showing relative positions of the IVC, BVC, and LVC. The black and dashed blue lines are the mean and median spectra, respectively (left y-axis). The dotted blue line is the standard deviation spectrum (right y-axis). Our analysis focuses on velocity channels to the right of the dashed gray line.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The TPFs of KIC 3440495 and the basic photometry mask. Top three panels: the target, the aperture mask, and background mask of S40 for the photometry from left to right. Bottom three panels: those of S41.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Residuals were imaged after the subtraction of the Fourier transform of the different disk models. The black contours represent ±3, 5, 10, and 20σ residuals.The gray dotted lines represent the original disk emission at 20, 50, 100, and 200σ. In each pair of panels, the left panel represents the 1.3 mm residuals with σ 6 = 54 μJy, and the right panel shows the 0.87 mm residuals with σ 7 = 110 μJy. Aside from the Gaussian disk model, the three other model residuals are remarkably consistent and similar, albeit with small differences, and generally display positive residuals at the disk’s four corners.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: (a) ALMA 1.3 mm field for VLA 1623W where VLA 1623Aa, Ab & B (left sources) have been subtracted. The residuals from Aa, Ab, & B are on the order of 3–5 σ 6 while the original emission from Aa, Ab & B, shown by the gray contours (20, 50, 100, and 500 σ 6), peaks at 930 σ 6 (Aa & Ab) and 980 σ 6 (B). On the right, VLA 1623W, is found to peak at 220 σ 6. (b) ALMA 1.3 mm deprojected and Aa, Ab, B-subtracted uv visibilities centered on VLA 1623W using an inclination of 80.°3 and a PA of 10.°3. The uv visibility profiles always display the full data for completeness. At 1.3 mm only the first binned data point is below 50 k λ, located at 40 k λ. (c) Same as panel (b) but for the 0.87 mm data. At 0.87 mm only the first binned data point is below 50 k λ, which is located at 20 k λ.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Real uv visibility profiles in black data points fit by a series of different disk models, described in Section 2.2, shown by the red lines; see Table 1 for the best-fit parameters shown here. The first left column shows the full 1.3 mm data while the second column shows a zoom in to highlight the region of structured visibilities. The third and fourth columns display the same information for the 0.87 mm observations. The topmost row shows the standard Gaussian disk model, the second row shows the Gaussian disk, gap model, the third row shows the Gaussian, disk, gap, ring model, and the fourth and final row shows the FTG model.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Brightness and real uv profiles for the frank fits to both data sets. In the top row the 1.3 mm data are fit and in the bottom row the 0.87 mm data are fit.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The amplitude spectra of KIC 3440495 from the Kepler and TESS data.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The light curves of KIC 3440495 made from the Kepler and TESS short- and long-cadence data. Note the difference of y-axis scales in the panels.
Paper: Detectability of Rotational Modulation in Kepler Sun-like Stars as a Function of Age
Authors: Kento Masuda
Figure caption: Fraction f of stars with detected rotational modulation as a function of mass and age, for the isochrone-only sample in Section 3.1. The filled vertical shaded region (violins) shows the posterior PDF for f in each age–mass bin, where the results from two mass bins are combined here. The blue circles and vertical error bars show the peaks and 68% highest-density intervals of these PDFs, and the short horizontal gray dashed lines show their means. The tan dashed line shows the f–t ⋆ relation predicted by the simple detection model; see the text in Section 5.
Paper: Detectability of Rotational Modulation in Kepler Sun-like Stars as a Function of Age
Authors: Kento Masuda
Figure caption: Same as Figure 12, but for the joint isochrone and gyrochrone sample defined in Section 3.2.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): GOES X-ray light curves; the shaded regions correspond to the times overlapping with the radio observations. Panel (B): dynamic spectrum of the solar-disk integrated flux densities for the two 15 minutes data sets. Due to limitations in data volumes, we omit the middle 5 minutes of data in the analysis. Panel (C): frequency-averaged time series of the flux densities for the eight frequency bands. Note that the time intervals between the left and right columns are different.
Paper: Detectability of Rotational Modulation in Kepler Sun-like Stars as a Function of Age
Authors: Kento Masuda
Figure caption: Age–mass distribution for the isochrone-only sample defined in Section 3.1 (left column) and the joint isochrone and gyrochrone sample defined in Section 3.2 (right column). From top to bottom, the two-dimensional age–mass distribution (mean of the posterior), marginalized mass distribution (mean and standard deviation), and marginalized age distribution (mean and standard deviation) are shown.
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Panel (A): composite EUV images for 171 Å (blue), 193 Å (green), and 211 Å (red); CHIMERA coronal hole boundary is shown as white contours. Panel (B): Helioseismic and Magnetic Imager magnetogram at 18:46:09 UT.
Paper: Detectability of Rotational Modulation in Kepler Sun-like Stars as a Function of Age
Authors: Kento Masuda
Figure caption: Top panel: spot-modulation amplitudes normalized by Kepler photometric precision and T eff of stars for which rotational modulation has been detected in the searches by Mazeh et al. (2015; open orange circles) and by McQuillan et al. (2014; gray dots); see the text for details of the samples. Bottom: normalized cumulative distributions for the normalized modulation amplitudes in the two samples shown in the top panel.