adsabs/AstroCLIMB huggingface dataset:
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Identifying candidate flaring regions: for every science-quality image, ALEXIS finds all pixels that are 90% of the maximum of that image. The first density-based clustering is applied to each image. Spatial clusters are designed to return the mean coordinates of a cluster with a minimum of one member located within the radius of 50″. The second clustering collapses the results of spatial clusters in the time dimension. Temporal clusters are designed to find regions that are bright for at least 15% of the total amount of images available within a radius of 50″. Finally, the wavelength dimensions are collapsed and we begin hyperspectral clustering. This will return the coordinates of long-lasting bright regions that occur in at least three-quarters of the available wavelengths. This process may return one or more candidate flare coordinates.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Data representation of a grid-searched Cartesian product: sample of training matrices for six zoomed-in Cartesian products and the grid-search tuple of two regions. ALEXIS searches for a C7.4-class flare that occurred at 22:31 UTC on 2014 January 7. Training matrices as seen by AIA-131 Å (L) paired to the GOES15-XRS-B target signal (Z). Each plot shows the normalized flux as a function of time. The title of each plot shows the cluster tuple with the specific zoom-in for each cluster. Maroon (XRS data), blue (integrated flux for region 1), orange (integrated flux for region 2). Upper row: no low-pass filter applied. Changes in exposure time predetermined by the AIA cause the signal to change value quickly. The signal is not smooth. Lower row: low-pass filter applied. The effects in the integrated flux from saturated pixels and nonsaturated pixels affected by the exposure time changes are filtered out; the signal is smoothed but the overall timing of peaks and valleys are retained. ALEXIS identifies two flares: a C8.4 flare happens at the orange candidate region and an M1.5 flare occurs at the blue candidate region.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Regularization path: we are interested in LASSO regression to eliminate candidate regions that are unnecessary. Column (1): X-ray and linear combination vector. Light red follows the target XRS signal with light orange and light blue, showing the individual weighted flux from the candidate regions. In gray, we show the predicted vector. Column (2): regularization path. Light orange and light blue show the value of each respective coefficient across the regularization path. The green vertical line indicates the λ value that produces the coefficients that created the predicted vector (gray); the green vertical line will progress through the values of λ from 10−3 to 10. Columns (3)–(4): the value of different evaluation metrics at each point in the regularization path. For each value of λ, we compute differences between the predicted vector (﹩\hat{Y}^{\prime} ﹩) and the XRS target signal (﹩\hat{Y}﹩). Here, we show how the Pearson correlation coefficient, rms error, mean square error, a least-squares model over the predicted signal, and its total energy differs as λ increases.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Which multipixel wavelengths and XRS telescopes return the best optimized fit? The single-pixel GOES15-B combined with the multipixel SDO 131 angstrom multipixel image returns the best fit. What degree of regularization is needed for this sample? Possible regularization values span 50 rational numbers sampled from a logarithmic space from 10−3 to 101. Within the bin for λ < 2 × 10−3 lies 36% of the sample, indicating a small degree of regularization needed for one-third of the sample. The average λ is 0.09 ± 0.16, suggesting that there is a large spread of regularization values. Regularizing our fit is a technique that produces more general models.
Paper: ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays
Authors: Jorge R. Padial Doble, Kelly Holley-Bockelmann
Figure caption: Distribution of flares by GOES class that ALEXIS is tasked with finding; 1000 random time ranges are chosen. The SWPC catalog returns 648 C-class flares, 378 M-class flares, and 35 X-class flares (1061 flares in total). SolarSoft returns a total of 653 C-class flares, 381 M-class flares, and 35 X-class flares (1069 flares in total). Note that all reported X-class flares between 2010 May and 2020 May are included in this iteration of the ALEXIS pipeline. In general, we assume SolarSoft uses the flares produced by the original SWPC catalog. Upon visual inspection, SolarSoft reports 11 false positives and the SWPC reports two false positives.
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: Summarization of molecular detectability (with ﹩\gt 3{\sigma }_{{\rm{\det }}}﹩) over three transits for four different subclasses of planets, using recent and upcoming ground-based spectrographs. The influence of cloudy atmospheres on molecular features and their detectability is highlighted. Additionally, the formation processes of the molecules at a specific pressure layer of 0.01 bar are discussed. Planetary visualizations are sourced from the NASA Exoplanet Catalog (https://science.nasa.gov/exoplanets/exoplanet-catalog/).
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: Correlation coefficient vs. velocity shift map for the 1.00 and 1.50 μm bands of NH3 and the 1.60 μm band of H2S across the atmospheres of Neptune-class planets, using future high-resolution spectrographs (Keck: magenta, TMT: teal, and E-ELT: gold) over three transits in cloud-free conditions. Each row corresponds to a specific planet (from top to bottom: HAT-P-11 b, HD 63433 c, K2-25 b, and TOI-270 d). These bands are detectable by all three instruments with enhanced sensitivity, highlighting the potential of future ground-based instruments to constrain nitrogen and sulfur chemistry.
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: Comparison of the high-resolution modeled spectra (R = 50000) of HAT-P-11 b, derived from the retrieved parameters in Y. Chachan et al. (2019), with the lower-resolution observational data in the HST WFC3 + STIS bandpass.
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: High-resolution transmission spectra for four planets, with a resolution akin to GINAO-B (R = 50,000) and full wavelength coverage for all spectrographs (0.4–2.45 μm). Each plot illustrates the spectra under two atmospheric conditions: clear (depicted in green) and cloudy (depicted in gold). The cloud model includes a gray cloud deck at 0.01 bar with a haze layer enhancing Rayleigh scattering scaled by a factor of 10. The band-wise contributions from individual molecules to the overall planetary spectra are also depicted.
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: High-resolution cross section for key species of interest plotted as a function of wavelength at 1641 K and 10−2 bar.
Paper: Quantified Estimation of Molecular Detections across Different Classes of Neptunian Atmospheres Using Cross-correlation Spectroscopy: Prospects for Future Extremely Large Telescopes with High-resolution Spectrographs
Authors: Dwaipayan Dubey, Liton Majumdar, Charles Beichman, Geoffrey A. Blake, Gautam Vasisht, Thomas Henning
Figure caption: VMR profiles for selected molecules in the atmospheres of four planets. Molecules were chosen based on having an average photospheric mixing ratio greater than 10−8. The pressure layers defining the photosphere boundary are 1 bar and 0.1 mbar in our case.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: Mixing-matrix elements of WFG for the HIGH-Z scenario. The left plot represents the diagonal matrix elements for two to five independent components. The right plot shows the matrix elements from the 48th row of the mixing matrix described in the second term of Equation (19). The gray-shaded regions represent a subset of frequencies tested for the leakage suppression. The dashed black line in the right panel represents the uniform weighting with an amplitude of 1/70.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: Mixing-matrix elements of WFG for the LOW-Z scenario. The left plot represents the diagonal matrix elements for two to five independent components. The right plot shows the matrix elements from the 20th row of the mixing matrix described in the second term of Equation (19). The gray-shaded regions represent a subset of frequencies tested for the leakage suppression. The dashed black line in the right panel represents the uniform weighting with an amplitude of 1/30.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: Cross correlations between H I and κ with the H I simulated directly from input theory (blue solid) and the component-separated H I (red solid). We assume that the κ field is only correlated with H I channels at a subset of frequencies. The left plot shows the cross-power spectrum of the 20th channel for the LOW-Z scenario, and the right plot shows the cross-power spectrum of the 48th channel for the HIGH-Z scenario. The colored dashed lines are different leakage terms calculated from Equation (19) with variations in the effective number of frequency channels. The results are obtained with ns = 4.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: Angular cross-power spectra for the HIGH-Z configuration at an effective redshift of 0.41 (channel 66) when κ is correlated with both all the H I channels (left) and only six channels (right), i.e., channels 46–51. In addition to the cross-power spectra with H I before (blue) and after (red) the foreground removal procedure, we also show the debiased cross-power spectra with Equation (24) (gray) and Equation (25) (orange), as well as a uniform weighting scheme (dashed red). The results are obtained with ns = 4.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: Angular cross-power spectra for the LOW-Z configuration with an effective redshift of 0.17 (channel 26) when κ is correlated with both all the H I channels (left) and only seven channels (right), i.e., channels 18–24. In addition to the cross-power spectra with H I before (blue) and after (red) the foreground removal procedure, we also show the debiased cross-power spectra with Equation (24) (gray) and Equation (25) (orange), as well as a uniform weighting scheme (dashed red). The results are obtained with ns = 4.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: The averaged signal-to-noise ratios (SNRs) per multipole (Equation (30)) from 100 realizations. In this figure, we show the SNRs at two different redshifts for both the LOW-Z  and HIGH-Z  scenarios. In particular, we compare the SNRs for cross correlations with the CMB lensing in red and with tomographic tracers in blue.
Paper: Investigating Cross Correlations between Cosmic Microwave Background Lensing and 21 cm Intensity Mapping
Authors: Alessandro Marins, Chang Feng, Filipe B. Abdalla
Figure caption: The SNRs per effective redshift or frequency channel. The effective redshift is taken as the mean redshift of a given channel. The shaded regions represent the galaxy-survey-like scenario where only a few H I frequency channels are correlated with the CMB lensing.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: ISN H maps for season 2009–2010 in energy bin 1 (two top rows) and bin 2 (two bottom rows) derived with the in-flight approach (first and third row) vs. the approach with α ≡ 1 everywhere (second and fourth row). The left column shows the derived ISN H intensity, the right column shows the corresponding relative uncertainties of the ISN H intensities (red pixels indicate places where the relative uncertainty exceeds 1, i.e., the ISN H intensity is ill constrained). The in-flight α-parameter data and uncertainties for both energy bins is available in a text file as data behind the figure. The data includes 15 yr of maps.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Map of raw H− in units of counts per second for energy bin 1 of ISN season 2. The upper 30 spin angles correspond to the ram hemisphere, the lower spin angles correspond to the antiram hemisphere of IBEX-Lo observations. The band of count rates at 15∘ spin angle is an electronics artifact. These count-rate maps are the basis to separate the ISN H signal (visible as blue pixels around orbit 70) from the count rates due to primary and secondary ISN He. No data were acquired during orbit 62.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: ISN H Mollweide maps in ecliptic coordinates for the ISN seasons 2009–2013 in energy bin 1. The left column shows the derived ISN H intensity in cm−2 sr−1 s−1 (identical color scale for all years), and the right column shows the corresponding relative uncertainties whereby red pixels indicate a relative uncertainty >1. These ISN H Mollweide maps and uncertainties are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Expected ratios of ISN He count rates in energy bin 1 to bin 3 (α(13)) and in energy bin 2 to bin 3 (α(23)) as a function of the mean energy of incoming ISN He atoms. The solid and dashed lines (in blue or red) correspond to the nominal and lower PAC voltages, respectively. The two laboratory calibration data points are shown as dots. We adopt a somewhat arbitrary limit at 40 eV, below which the response in energy bin 3 is too low to provide the basis for this analysis.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Ratio of H− count rates caused by ISN He in IBEX-Lo energy bins 1, 2, and 3 plotted against IBEX-Lo spin angle (180∘ ≃ ecliptic north pole, 270∘ ≃ ecliptic plane) for the example of orbit 70. The α(13) and α(23) values are based on the in-flight approach, thus depending on ISN He energy and ecliptic latitude; the simplistic approach assumes constant α values everywhere.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Comparison of algorithms for season 2009–2010: Longitudinal cross section of derived ISN intensities along maximum intensities close to ecliptic plane. Red symbols denote results from the in-flight approach, black symbols show results from the approach with α ≡ 1.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Comparison of algorithms for season 2009–2010: Latitudinal cross section of derived ISN intensities. Red symbols denote results from the in-flight approach, black symbols show results from the approach with α ≡ 1.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: ISN H Mollweide maps in ecliptic coordinates for the ISN season 2009–2010 for energy bins 1 (top row) and 2 (bottom row). The left column shows the derived ISN H intensity, the right column shows the corresponding relative uncertainties of the ISN H intensities.
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: ISN H Mollweide maps in ecliptic coordinates for the ISN seasons 2019–2023 in energy bin 1. The left column shows the derived ISN H intensity in cm−2 sr−1 s−1 (identical color scale for all years), and the right column shows the corresponding relative uncertainties whereby red pixels indicate a relative uncertainty >1. These ISN H Mollweide maps and uncertainties are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: Time series of ISN H flux (top) and solar activity (bottom). The top panel shows the total flux of ISN H in cm−2 s−1 between 11 and 21 eV (red data points) and between 20 and 41 eV (blue data points) for the year of observation. The data points of 2016 had to be skipped because only a fraction of the potential ISN H signal was covered. The bottom panel shows the number of sunspots as a proxy for solar activity (SILSO World Data Center 2024).
Paper: 15 yr of Interstellar Neutral Hydrogen Observed with the Interstellar Boundary Explorer
Authors: André Galli, Paweł Swaczyna, Maciej Bzowski, Marzena A. Kubiak, Izabela Kowalska-Leszczynska, Peter Wurz, Fatemeh Rahmanifard, Nathan A. Schwadron, Eberhard Möbius, Stephen A. Fuselier, Justyna M. Sokół, Jonathan Gasser, Jacob Heerikhuisen, David J. McComas
Figure caption: ISN H Mollweide maps in ecliptic coordinates for the ISN seasons 2014–2018 in energy bin 1. The left column shows the derived ISN H intensity in cm−2 sr−1 s−1 (identical color scale for all years), and the right column shows the corresponding relative uncertainties whereby red pixels indicate a relative uncertainty >1. These ISN H Mollweide maps and uncertainties are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The distribution of galaxies in the SFR–M* plane. The galaxies with local noise σ < 75 μJy are represented by filled dots, while the others are represented by empty dots. The blue dots indicate the FUDS0 H I galaxies, while red dots are non-detections. The black lines are the same as for Figure 15. The distribution of stellar mass (upper panel) and SFR (right-hand side panel) are given by the hatched histogram with the same color. The solid lines indicate the full sample.