adsabs/AstroCLIMB huggingface dataset:
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: The figure shows the time-frequency variation of Stokes I and linear polarization fraction (fL) for two noise storm sources. Rows 1–3 display Stokes I, fL, and its error, respectively, with white points indicating nondetections (I < 10σ or Q/U < 5σ). The bottom row shows the time variation of fL at 218.5 MHz. Rapid, source-specific changes in fL are evident. A type III burst at 04:14:14 UTC (marked by a red inverted triangle) in the eastern source leads to a sharp drop in fL from >10% to <5% at 217–220 MHz. These distinct variations confirm that the observed polarization is intrinsic to the solar emission and not of instrumental origin.
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: The top panel shows the cross-hand phase variation with frequency from the Centaurus A field. The bottom panels validate these solutions using J0351-2744. Linear and circular polarization maps at +33.958 rad m−2 are shown (bottom left and middle), with Stokes I contours at 20%, 40%, 60%, and 80% of the peak. The bottom right shows the 1D Faraday dispersion function for the eastern hotspot, peaking at +33.958 rad m−2 (blue). Residual circular polarization is at the noise level. The small offset from the catalog RM (+33.58 rad m−2) is likely due to uncorrected ionospheric RM.
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: Simultaneous detection of linearly polarized emission at 218 MHz from the MWA (top panels) and uGMRT (bottom panels). Two bright radio sources on the eastern and western limbs are marked in the left panels, with zoomed-in views shown in the middle and right panels. Red contours denote linear polarization intensity (L) at 0.4, 0.6, 0.8, and 0.9 of the peak, and black circles indicate the optical solar disk. Both sources show partial linear polarization. The eastern source, weaker in Stokes I, has a polarization fraction of 13.5% ± 0.5% (MWA) and 12.3% ± 2.0% (uGMRT). The brighter western source shows lower polarization: 6.0% ± 0.3% (MWA) and 5.9% ± 0.5% (uGMRT).
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: Comparison of Stokes I to Q and I to U leakage before and after the image-based leakage correction. The top panel shows the Stokes Q (left) and U (right) maps at 217 MHz before image-based leakage corrections were done. Regions with brightness temperature >106 K have been masked. The bottom panels show the corresponding Stokes Q and U maps after the application of image-based leakage correction. The black contour on each of the maps indicates the 5σ level in Stokes I. After applying this correction, the mean values of Q and U in the quiet-Sun region are 1.82 and -0.11 Jy beam−1, respectively, which are significantly lower than the rms values of 4.70 and 4.46 Jy beam−1.
Paper: First Robust Detection of Linear Polarization from Metric Solar Emissions: Challenging Established Paradigms
Authors: Soham Dey, Devojyoti Kansabanik, Divya Oberoi, Surajit Mondal
Figure caption: The figure shows the Stokes I (total intensity) dynamic spectra (top panels) and the time series of the band-averaged flux density (bottom panels) for 4 minutes of the event on 2022 June 22, captured by the MWA (left panels) and uGMRT (right panels). A type III burst took place at 04:14:14 UTC, which corresponds to the highest peak in the bottom panels.
Paper: The Importance of Dust Distribution in Ionizing-photon Escape: NIRCam and MIRI Imaging of a Lyman Continuum-emitting Galaxy at z ∼ 3.8
Authors: Zhiyuan Ji, Stacey Alberts, Yongda Zhu, Eros Vanzella, Mauro Giavalisco, Kevin Hainline, William M. Baker, Andrew J. Bunker, Jakob M. Helton, Jianwei Lyu, Pierluigi Rinaldi, Brant Robertson, Charlotte Simmonds, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Joris Witstok
Figure caption: Astrometry comparison. Filter names are labeled at the top of individual panels. The histograms show the difference (in arcseconds) between the centroid measured in each corresponding filter and the centroid listed in the JADES photometric catalog. The black histogram represents the difference in the x-direction, while the red histogram represents the difference in the y-direction. The standard deviations (in pixels) are also labeled in each panel.
Paper: The Importance of Dust Distribution in Ionizing-photon Escape: NIRCam and MIRI Imaging of a Lyman Continuum-emitting Galaxy at z ∼ 3.8
Authors: Zhiyuan Ji, Stacey Alberts, Yongda Zhu, Eros Vanzella, Mauro Giavalisco, Kevin Hainline, William M. Baker, Andrew J. Bunker, Jakob M. Helton, Jianwei Lyu, Pierluigi Rinaldi, Brant Robertson, Charlotte Simmonds, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Joris Witstok
Figure caption: The Hα of Ion1 is covered by both the F335M and F356W images, but it appears at the parts of the two filters with largely different transmissions, allowing us to derive the 2D Hα intensity map using the two NIRCam images (Appendix B).
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: (Top) Degree of (fractional) radius inflation for our study sample, determined in relation to standard, nonmagnetic, unspotted stellar isochrone models, as a function of the rotational Rossby number. Stars are color-coded and assigned a marker by their cluster membership. The black line is the fiducial “best fit” for the power-law relation, and the gray lines indicate alternate sampled solutions of the MCMC chain (representing the uncertainty of the solution), with the blue band representing the standard deviation of points about the best-fit line. Points that fall off the edges of the plot limits are denoted by triangle symbols but are still included in the fit. (Bottom) Observed radius inflation as a function of temperature suppression (left) and luminosity offsets from SPOTS isochrones (right). Temperature suppression is observed to correlate with radius inflation in a manner that preserves the luminosity.
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Magnetic starspot filling fractions as a function of the rotational Rossby number parameter for stars in our study sample. Stars are colored and assigned a marker according to their host cluster. For comparison, the light blue swathe represents the fitted relation found by L. Cao & M. H. Pinsonneault (2022) in their study of the Pleiades, which appears to trace the lower envelope of the spot–Rossby relation for our larger sample of open clusters with ages spanning 10–670 Myr.
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Direct comparison of the degree of observed radius inflation and predictions from the magnetic SPOTS models. Points are color-coded by starspot filling factor, and the marker shape corresponds to the cluster. Inset plot shows the residual in the observed radius inflation parameter relative to model predictions. Bottom plots show the mean relation with just the individual stars of each cluster. The robust 1:1 correlation between the observed inflation values and the predicted values suggests that the magnetic stellar evolution model makes consistent radii estimates of inflated stars. Two points from Upper Sco (indicated by red upper limits) are not shown on the diagram, but they are still included in the fit.
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Comparisons of radii and temperatures recovered for individual stars with those predicted by the SPOTS models, as a function of fspot. Markers are colored by their fspot and lines are also colored by the corresponding fspot theoretical starspot isochrones from SPOTS. Inset plots relate the observed fspot recovered from the spectra (x-axis) to the spot filling fraction inferred from the isochrones using the measured radii (y-axis).
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Markov Chain Monte Carlo corner plots showing parameters recovered for the power-law fit in Figure 2. The best-fit values are, for rotational saturation: ﹩\mathrm{log}{{\rm{Ro}}}_{{\rm{crit}}}=-1.39{6}_{-0.070}^{+0.076}﹩; spot saturation level: ﹩{f}_{\mathrm{spot},\mathrm{sat}}=0.27{6}_{-0.016}^{+0.017}﹩; slope at ﹩\mathrm{log}{\rm{Ro}}\gt \mathrm{log}{{\rm{Ro}}}_{{\rm{crit}}}﹩: ﹩{m}_{{\rm{slope}}}=1.15{4}_{-0.081}^{+0.087}﹩.
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Binary rejection procedure on the clusters included in this analysis. Marker sizes correspond to the measured starspot filling fraction and are shown overlapping in the event that individual stars are excluded due to one or more factors.
Paper: The Relationship of Stellar Radius Inflation to Rotation and Magnetic Starspots at 10–670 Myr
Authors: Lyra Cao, Keivan G. Stassun
Figure caption: Markov Chain Monte Carlo corner plots showing parameters recovered for the linear fit in Figure 4. The best-fit values are described in Section 3.3.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The left panel shows a comparison between the JWST MIRI/MRS and Spitzer/IRS disk spectra of HD 23514 taken 15 yr apart with the bottom one showing the flux ratio between the two. The color shaded area indicates the associated ±1σ uncertainty. The two spectra agree within ±1σ in the silica 9 μm region while in the 20 μm region JWST data appear to be slightly lower by ∼3σ. The thin green line is the estimated dust continuum of the JWST data (for details see Section 3.3). The right panel depicts the derived dust emissivity spectrum in comparison with a silica-rich protoplanetary disk (PPD; orange, dotted–dashed line), and a typical interstellar medium (ISM)-like, very low-crystallinity dust mineralogy (blue dashed line; see Appendix A for details).
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The photodissociation lifetime of unshielded molecules as exposed to both the UV photons from HD 23514 and the interstellar radiation field (ISRF) as a function of stellocentric distance where the dashed lines are those only using ISRF. The UV emission from the star was estimated using the Kurucz model (Appendix A.1), which under estimates the amount of UV photons given its youth. The unshielded photodissociation lifetimes shown here should be considered as upper limits.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The SED of the HD 23514 system where the data points come from 2MASS, Spitzer, and Herschel photometry along with the mid-IR spectra. Lines show the SED models for a disk in a radial range of 0.1–3 au, a dust composition mixture of silica and pyroxene, and grains lacking insipid features. The prominent 10 μm and 20 μm features mostly come from optically thin silica and pyroxene grains within sub-astronomical-unit distances (for details see Section 4.1 and Appendix D.1).
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: Zoom-in, continuum-subtracted spectrum centered at ∼15 μm showing the dominant CO2 Q-, P-, and R-branch molecular lines in the upper panel and the residuals (data − model) in the bottom panel. The black line depicts the data, with the gray horizontal area showing the ±1σ estimated in the local spectral region. Filled, color areas show the model emission from four volatile species: CO2, H2O, NH3, and 13CO2, with the dark gray area showing the model sum.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: Spitzer IRS low-resolution spectrum of HD 23514 observed in 2008 centered at the CO2 15 μm complex, where the data are shown as the black line with the 1σ rms error showing as dark vertical lines (gray for the combined error). The thick red line is the expected, low-resolution model spectrum if the same level of the CO2 emission detected by JWST (thin red line) was also present. This comparison suggests that the same CO2 emission is presented in the Spitzer spectrum where the brightest Q-branch line is detected at 4.3σ.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The IR variability around HD 23514 as monitored by warm Spitzer in ∼3 day cadence when available. The upper panel shows the excess fluxes obtained by the two shortest IRAC bands while the bottom depicts the color temperatures derived by the flux ratio. The system exhibits stochastic, weekly variability without obvious periodicity. There exists a weak, positive trend between the excess flux and color temperature.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: MIRI MRS data before (red) and after (blue) stellar photosphere subtraction. The gray line represents the featureless dust continuum with a combination of two blackbody emissions at 750 K and 200 K. This featureless dust continuum was used to compute the dust emissivity as shown in the right panel of Figure 1.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: Similar to Figure B2 but with WISE W1 and W2 data along with the Spitzer/IRAC I1 and I2 photometry taken in 2008, showing yearly IR variability. The lowest 3–5 μm flux appeared to be in 2015. The two epochs of mid-IR spectra obtained by Spitzer and JWST are also indicated.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: IR photometry of HD 23514 available in the literature/archive before 2013 in comparison with the Spitzer/IRS spectrum. The horizontal bars show the bandpass of the measurement while the vertical ones for the 1σ uncertainty.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The posterior distributions for the CO2 fitting using the three parameters: emitting area (log A in units of au2), column density (log N in units of cm−2), and gas temperatures (log T in units of K).
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The left panel shows the estimated thermal equilibrium dust temperature as a function of stellocentric distance from HD 23514 under the optically thin condition. Line styles depict different compositions with red for 0.1 μm and blue for 1 μm grains. The thick gray line represents the temperature of a blackbody emitter. The right panel shows the expected SED for 0.1 μm silica grains at different (colored) temperatures normalized at the 20 μm peak, illustrating that the contrast/ratio between 9 μm and 20 μm is sensitive to the dust temperature.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: The continuum-subtracted spectrum of HD 23514 centered at the CO gas (upper for the low Tgas and lower for the high Tgas models; for details see Appendix C). The shaded color regions show the slab model predictions of CO (purple) and others (same as Figure 2). For all the comparison plots between the data and model, the flux panels are shown starting from −2 rms to 1.5 times the peak flux in the displayed segment and the residual panels are all shown in the range of ±4 rms.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: Same as Figure C2 for different spectral segments with different molecules using the same plotting rules.
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: Computed β values, the ratio between radiation-pressure and gravitational forces, for different sizes and compositions of ideal dust grains around HD 23514. The horizontal dashed line marks β = 0.5 where the blowout size is defined and grains above the line are subject to radiation-pressure blowout (details see Appendix D.2).
Paper: Discovery of Volatile Gas in the Giant Impact Disk Around the 150 Myr Old HD 23514
Authors: Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner
Figure caption: CO2 shielding efficiency (in terms of factors to prolong the photodissociation lifetime) from different molecules (colored) against photodissociation as a function of column density. Solid lines show the ISRF as the radiation field while the dashed ones show solar radiation.
Paper: Observability of Isolated Stellar-mass Black Holes
Authors: Lena Murchikova, Kailash C. Sahu
Figure caption: Estimated emission spectra of an IsoBH located 50 pc from the Sun, accreting gas from four types of local ISM: cold dense cloud with a density of ∼3000  cm−3 (cyan), clumps within Local Interstellar Clouds with a density of ∼20 cm−3 (orange), warm partially ionized medium with a density of ∼0.3 cm−3 (yellow), and hot ionized coronal gas (gray). Other types of Galactic ISM are not present within 50 pc of the Sun. The thin dotted lines show the expected emission spectrum from an IsoBH accreting at the Bondi rate (λ = 1), representing the upper limit of the emission. The thick solid lines below the dotted lines, shown in corresponding colors, represent the spectrum from the IsoBH accreting at a more realistic 1% of the Bondi rate (λ = 0.01). The exaggerated thickness illustrates large uncertainties in the accretion-model parameters. Note that some of the thin dotted lines overlap with the thick solid lines of other colors. We only plot the upper limit for the coronal gas corresponding to the Bondi rate, as the emission is already too low to be detectable. For convenience, we show the spectra in two different units (νFν and Fν) commonly used in different wavelength regions. Dark gray lines indicate the observational sensitivities of Chandra, JWST, ALMA, and SKA, achievable within the integration times listed in brackets.
Paper: Observability of Isolated Stellar-mass Black Holes
Authors: Lena Murchikova, Kailash C. Sahu
Figure caption: Estimated emission spectra of an IsoBH located 10 kpc from the Sun and accreting from the core of a GMC with densities 106 cm−3 (yellow), and a core of an ordinary MC with density 104 cm−3 (gray). The thin dotted line shows the expected emission spectrum from an IsoBH accreting at the Bondi rate (λ = 1), representing the upper limit of the emission. The thick solid lines below the dotted lines, shown in corresponding colors, represent the spectra from the IsoBH accreting at a more realistic 1% of the Bondi rate (λ = 0.01). The exaggerated thickness illustrates large uncertainties in the accretion-model parameters. For convenience, we show the spectra in two different units (νFν and Fν) commonly used in different wavelength regions. Note that the dotted gray line overlaps with the thick yellow line. Thin dark gray lines indicate the observational sensitivities of Chandra, JWST, ALMA, and SKA, achievable within the integration times listed in brackets.
Paper: Observability of Isolated Stellar-mass Black Holes
Authors: Lena Murchikova, Kailash C. Sahu
Figure caption: Estimated emission spectra of an IsoBH located 200 pc from the Sun, accreting gas from three types of local ISM: MCs with an average density within the core of ∼104 cm−3 (gray), cold dense clouds with a density of ∼3000 cm−3 (cyan), and gas clumps within Local Interstellar Clouds with a density of ∼20 cm−3 (orange). Other types of medium, such as warm medium and coronal gas, are also present within 200 pc from the Sun. However, a 10M⊙ IsoBH located at 200 pc in such a medium would be undetectable (as evident from Figure 1), hence we do not show them here. The thin dotted line shows the expected emission spectrum from an IsoBH accreting at the Bondi rate (λ = 1), representing the upper limit of the emission. The thick solid lines below the dotted lines, shown in corresponding colors, represent spectra from the IsoBH accreting at a more realistic 1% of the Bondi rate (λ = 0.01). The exaggerated thickness illustrates large uncertainties in the accretion-model parameters. Note that some of the thin dotted orange line overlaps with the thick solid cyan line. For convenience, we show the spectra in two different units (νFν and Fν) commonly used in different wavelength regions. Dark gray lines indicate the observational sensitivities of Chandra, JWST, ALMA, and SKA, achievable within the integration times listed in brackets.