adsabs/AstroCLIMB huggingface dataset:
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption:                         Long-term 0.9 m light curves for the three true twin systems. A (top) and B (bottom) components are shown for each pair, with a brightening trend indicated by a rise in each plot. Observation filters are noted in each subplot title. GJ 1183 A and B are shown spanning over a decade of coverage, while the other two systems capture several years. Note the very different y-axis scale for 2MA 0201+0117 A and B. Year times are the Julian epoch, i.e., J2000 plus the number of Julian years since then. Large clusters of points in 2022 for 2MA 0201+0117 AB and 2023 for GJ 1183 AB are from the additional rotation visits analyzed in Figure 6, with moderate flaring points left included here as examples. Open circles represent visits when only a single frame was secured; these are excluded from all quantitative analyses. Black numbers in the upper left of each panel are the mean absolute deviation (MAD) values (average of absolute value offsets from the mean) for the solid points for each component. Gray numbers in the top right of each panel are the average noise levels of the nonvarying reference stars used in the differential photometry analyses, again calculated as MAD values; these noise levels are indicated visually as gray shaded regions above and below 0 in each panel. The light-curve data are available as Data behind the Figure (DbF) products. (The data used to create this figure are available in the online article.) (The data used to create this figure are available.)
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: Optical images of the NLTT 44989 AB system, showing the relative positions of the brighter target M dwarfs and fainter background contaminating sources. The left panel shows a DSS2-Blue image taken roughly half a century ago (Ep. ≈ 1975; B. M. Lasker et al. 1996; R. R. Gal et al. 2004), and the right panel shows a VPHAS DR4 g-band image taken more recently, about a decade ago (Ep. ≈ 2012; J. E. Drew et al. 2014). Red squares and blue circles show the relevant source positions from Gaia DR3 at J2000 and J2016, respectively, with green arrows along the proper-motion vectors of the twin stars—the background sources have negligible proper motions. Our new observations of the system span 2019–2024, when proper motion has moved B farther on top of background source 1. Several other background sources in Gaia DR3 are not shown in these images for visual clarity, but all are negligibly faint and/or resolved from our target stars. See Sections 3.6 and 3.6.1 for a discussion of the small contamination impacts in the various observations we use.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: An observational Hertzsprung–Russell Diagram using Gaia DR3 magnitudes and parallaxes. Gray points show a sample of Gaia sources within 50 pc to illustrate the main sequence. Large black circles indicate stars in our sample of 36 M dwarf twin binary pairs. The four systems examined in this paper are filled in and labeled, with red lines connecting the two components in those pairs. A diagonal cyan line represents the gap marking the transition between partially and fully convective M dwarfs near ∼0.35M ⊙ (W.-C. Jao et al. 2018, 2023), offset downward by 0.05 mag to approximately match the middle of the gap instead of the upper edge.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: Blue data points show the observed Chandra coronal X-ray spectrum from 0.3–10 keV for the β Pic Moving Group members 2MA 0201+0117 A and B, grouped to 9 counts per bin. Overplotted in orange are the forward-folded best-fit APEC models; A uses a single-temperature component whereas B uses a two-temperature component in the coronal model. The bottom panels show the residual values divided by the errors, with horizontal bars indicating the energy bin widths. Spectral fits for all of the other quiescent X-ray data sets can be seen in Figure 17 in the Appendix.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: A background-subtracted Chandra X-ray light curve for NLTT 44989 B, showcasing a strong stellar flare during the exposure. Vertical dashed blue lines indicate the time period used for isolating the stellar flare. Counts are merged into 200 s bins. Light curves for all of the other X-ray data sets can be seen in Figure 16 in the Appendix.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: The temporal variation of spectral parameters T4, EM4, Z, and Luminosity LXF for sets S1 and S2. The T4 is in units of MK, EM4 in 1053 cm−3, LXF in 1031 erg s−1. The shaded regions show the peak phase of the corresponding flare.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: The density vs. temperature (n–T) plot, where EM1/2 is considered as the proxy of density. ζ is the slope of the n–T diagram from the decay phase of the flares (a) F1, (b) F2, and (c) F3.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: All the elemental abundances relative to Fe are plotted against the first ionization potential (FIP). The values are provided in Table 7.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: X-ray light curves of HR 1099 in different detectors. The flaring regions are marked by the vertical lines.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: Log–log plot of flare duration vs. luminosity with linear curve fit.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: The RGS1 and RGS2 spectra of pre-flare state P4 and flare F3 are shown in the upper panel with 3-T VAPEC and 4-T VAPEC models, respectively. The lower panel shows the residual of the modeled spectra.
Paper: Characterizing Superflares in HR 1099 Using Temporal and Spectral Analysis of XMM-Newton Observations
Authors: Shweta Didel, Jeewan C. Pandey, A.K. Srivastava
Figure caption: Soft and hard X-ray light curves along with the HR curve with 100 s binning.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: 2D power spectra of WWZ, light curves, eclipse depth, and O – C diagram of LT Eri. (a) The WWZ 2D power spectra of the out-of-eclipse light curves, with the red dotted line representing the orbital period. (b) The solid black circles indicate the original light curves, and the red curves show the LOESS fit used for detrending. (c) The detrended light curves, with the black solid circles representing the out-of-eclipse data. (d) A plot of eclipse depth vs. time, with the solid red line representing the LOESS fit. (e) The residuals of the LOESS fit from panel (d), with the red solid line showing the sine fit. (f) The original O – C diagram of LT Eri, with the magenta dots indicating the O – C values during quiescence, and the blue dotted line showing the sine fit to the magenta dots. (g) The O – C diagram of the reconstructed light curves; see Section 3.7 for details.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: (a) The upper panel shows the LSP of the light curve after removing the outburst trend, and we use the symbol Ω for the frequency of the orbital period and its harmonics. The bottom panel is the LSP of the out-of-eclipse curves. On the right, an enlarged view of the yellow-highlighted region is shown, with the red and blue vertical lines indicating the positions of the orbital period and the NSHs, respectively. (b) The solid green line is the parabolic fit to the eclipse curve with a phase width of 0.16; the solid red line is the sine fit to the out-of-eclipse curves; and the blue dotted line is the intersection of the minima with the parabolic fit and the sine fit, respectively.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: All light curves and outburst analyses for LT Eri. (a) Light curves from TESS, ZTF, ASAS-SN, and AAVSO are shown, with the sine fit indicated by the fluorescent line in the shaded gray region. (b) Comparison of different outbursts: the symbols correspond to those in panel (a). The numerical codes begin with JD, with the vertical red dashed line marking zero, and the yellow shaded area represents the range from −5 to 5 days. (c) LSP results for all light curves; the solid red line is the Gaussian fit. (d) For the folding curves of the long and short outbursts in panel (b), the yellow areas on the left and right span 18 and 10 days, respectively.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: (a) The left and right panels display the folding curves of LT Eri during quiescent and outburst phases, respectively, utilizing a folding period of 0.16265161(7) days. (b) The panel illustrates the out-of-eclipse curves of LT Eri during the quiescent phase and the decline of the outburst. (c) Phase-folded light curves of LT Eri during the quiescent phase. The solid red line represents the LOESS fit, with a folding period of 0.170202916(63) days. (d) Folding curves of the residuals in panel (b).
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: Sine fit and LSPs for seven different segments. Left: seven different curves—the black solid circles show the out-of-eclipse curve, the black hollow circles show the eclipse part, and the red curve represents the sine fit. Right: the LSP corresponding to the out-of-eclipse curves on the left; the red vertical dotted line is the orbital period.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The radial encircled energies for the imaging (left) and coronagraphic (right) bands. Subsequent bands are offset by a factor of 0.1. Multiple radial encircled energies are plotted for each band using repeated observations except F2550W, which is based on the WebbPSF model at all radii. The black points give the radii for 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, and 0.85 encircled energies with their uncertainties as horizontal lines. The radii uncertainties are based on the scatter of the radii computed from independent observations. The coronagraphic profiles are broader than the imaging profiles, and the Lyot F2300C profile is narrower than expected given an extrapolation of the behavior of the three 4QPM coronagraphic profiles (F1065C, F1140C, and F1550C). This is due to the difference in type of coronagraph.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The F1280W calibration factors plotted as a function of the source predicted flux density, measured background, observation time, and source type. The calibration factors are corrected for the time and subarray dependencies. Each point represents one observation for one star. The colors and symbols to distinguish different types of stars and subarrays are the same in all panels. While the observation of HD 180609 is within the scatter for this band, it is flagged and not used (Section 3.2). In addition, one observation is flagged as >3.5σ from the weighted average and not used (Section 3.2). The solid horizontal gray line gives the weighted average in each panel, with the ±1σ standard deviations as dotted gray lines. The average calibration factors and uncertainties are given in the lower right of each plot. The percentage standard deviation and standard deviation of the mean are given in parentheses as well.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The fractional change in flux density relative to SUB256 for each subarray using a variety of observations. The dedicated subarray transfer observations taken in F770W and F1280W are simple ratios of the measured flux densities where multiple measurements in the same subarray were averaged if available. All of the flux-calibration observations were used to measure equivalent ratios using the weighted-average calibration factors for each subarray and band. The uncertainties for these ratios are the weighted standard deviation of the mean. No error bars are shown for three or fewer observations. The blue stars are the adopted relative subarray throughputs.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Left: the time-dependent behavior of the repeated observations of BD+60 1753 plus two other stars for all the imaging filters. An exponential model fit to the observations in each band is plotted in this panel as the solid purple line. The dotted line gives the value after the modeled exponential has fully decayed. The amplitude A, the time constant τ, and standard deviation σ around the exponential fit are given on the left. Right: the residuals after subtraction of the exponential model.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: A visualization of the photometric method for GSPC P330-E observed with the F1000W imaging band with the BRIGHTSKY subarray. The full mosaic is shown on the left with a white and black box surrounding the target. The right panel zooms in on the target region with the aperture in white, the sky annulus in blue, and the final centroid position marked with a cross. The x- and y-axis units are pixels, which are 0.″11 across. The minima and maxima of the color scales differ between the two images.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Example images for the imaging and coronagraphic filters to illustrate the data quality and general characteristics of MIRI point-source observations. The targets include BD+60 1753 for the imaging bands from F560W to F1280W, δ UMi for the rest of the imaging bands, and HD 2811 for the coronagraphic bands. The image in the neutral-density filter (FND) is smoother compared to the other imaging bands due to its wide bandpass. The coronagraphic observations were taken well away from the coronagraphic centers, and so these are the unocculted PSFs.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The calibration factor vs. the detector parameters central-pixel rate, integration time, central-pixel well depth, and subarray. The calibration factors plotted have been corrected for the temporal and subarray dependencies. Different colors and symbols indicate different types of stars and subarrays. While the observation of HD 180609 is within the scatter for this band, it is flagged and not used (Section 3.2). In addition, one observation is flagged as >3.5σ from the weighted average and not used (Section 3.2). The horizontal gray solid line shows the weighted average, with dotted lines for the ±1σ standard deviation. The calibration factors and uncertainties are given in the lower right of each plot. The percentage standard deviation and standard deviation of the mean are given in parentheses as well.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The calibration factors as a function of model flux densities for every observation for the imaging and coronagraphic filters. The temporal response loss and subarray variations have been corrected. While the observations of HD 180609 are within the scatter for some bands, it is flagged in all bands and not used (Section 3.2). In addition, some observations are flagged as >3.5σ from the weighted average and not used (Section 3.2). A horizontal solid gray line and the parallel dotted lines give the weighted average ±1σ standard deviation. The calibration factors and uncertainties are given in the lower right of each plot, and the percentage standard deviation and standard deviation of the mean are given in parentheses as well.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The delivered calibration factors used by the pipeline are plotted vs. time for all bands except FND. The FND calibration has been determined for the first time with this work and so is not plotted. For the two most recent deliveries, the time-dependent variation is shown as a solid symbol (start of observations) connected to an open symbol (asymptotic value after all expected change). The changes reflect the improved calibration factor measurements with more observations and a better understanding of the telescope and instrument.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: The ratio of the average calibration factor for each band for each source type vs. the average calibration factor per band for all source types. Only bands with >3 individual measurements are shown as this is required to measure an uncertainty. The error bars for the individual bands are 1σ standard deviations. Black stars and vertical lines depict the weighted average of all bands and 5 times the standard deviation of the mean (5σ).
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Same as Figure 10 except plotted vs. source type.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Same as Figure 10 except plotted vs. central pixel rate.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Same as Figure 10 except plotted vs. central pixel well depth.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Same as Figure 10 except plotted vs. measured background.
Paper: The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy
Authors: Karl D. Gordon, G. C. Sloan, Macarena Garcia Marin, Mattia Libralato, George Rieke, Jonathan A. Aguilar, Ralph Bohlin, Misty Cracraft, Marjorie Decleir, Andras Gaspar, Sarah Kendrew, David R. Law, Alberto Noriega-Crespo, Michael Regan
Figure caption: Same as Figure 10 except plotted vs. observation time.