adsabs/AstroCLIMB huggingface dataset:
Paper: Adaptive Detection of Fast-moving Celestial Objects Using a Mixture-of-experts and Physical-inspired Neural Network
Authors: Peng Jia, Ge Li, Bafeng Cheng, Yushan Li, Rongyu Sun
Figure caption: The structure of the neural network used in E1.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: (a)–(c) Median maps of the brightnesses of individual J, H, and K bands along wavelength, multiplied by r2 with r being the radius around the predicted stellar position. The color scales are in units of Jy pixel−1 arcsec2. For comparison, the corresponding 0.8 μm brightness distribution is indicated by black contours (see Figure 2 for details). Black straight dashed lines correspond to the locations of searchlight beams identified in the HST images taken in 2011 and 2016 (H. Kim et al. 2021). The red circle in each panel indicates the radius at which the radial profile of the map changes it slope; beyond this radius, the radial profile either gets flattened or starts decreasing with increasing radius. (d)–(f) Radial profiles of the above panels along the R.A. and decl. directions (thick and thin lines, respectively). The horizontal dashed line in blue indicates the median value of the map. The vertical dotted lines in red correspond to the radius of the red circle in the above panel. (g)–(i) Azimuthal profiles of the maps in (a)–(c) as a function of the position angle, measured from north to east. Vertical dashed lines indicate the position angles of the searchlight beams depicted in the top panels. The horizontal dotted line in each panel presents the mean value of the profile.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Spectroscopic indices derived from our Gemini-NIFS spectro-imaging data on the central region of circumstellar envelope of CW Leo: the stellar position (red), an offset position (blue; 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩2 to the north), and the integration over the field of view (green). The corresponding indices of a sample of carbon stars are marked by black filled and open circles, which are separated by the black solid line drawn in the top left panel for the DIP153 indices (see A. Gonneau et al. 2016). Vertical bars indicate uncertainties propagated from the residual standard errors of the fits for individual continuum determinations. Magenta and cyan dashed lines represent polynomial fits of degree two for the template carbon stars marked by filled and open circles, respectively, excluding three outliers at (J − K) < 1 and >4. The star V CrA at (J − K) = 4.3, which was excluded during the fit, still follows the fitting results (magenta dashed lines).
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Velocity lag derived from cross correlations of CO overtone bands observed in the range of 2.293–2.420 μm. (a) The measured velocity map in a linear color scale from 0 to 16 km s−1 shows an overall increase with radius from the expected stellar position, but also displays anisotropy. The radii of the black circles are 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩2, 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩5, 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩0, and 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩3, respectively. (b) The profiles along the west–east (blue) and south–north (red) cuts, including the stellar position at the center, are obtained from the (a) panel. The expansion velocity curves of the wind of CW Leo suggested by J. P. Fonfría et al. (2008, F08) and L. Decin et al. (2015, D15) are plotted by dashed and dotted lines, for comparison. (c) The velocity lag profiles as a function of position angle are measured at different radii.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Maps of the spectroscopic indices (a) DIP153, (b) COH52, and (c) CO12, showing meaningful variation within the scale of the observed image. The corresponding 0.8 μm brightness distribution is marked by black contours, same as in Figures 2 and 4. Red circle indicates a radius of 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩2 from the center, at which wind acceleration occurs (L. Decin et al. 2015). White contours show the levels of 0.20 and 0.23 of the spectroscopic index map in the (a) panel, 0.11 in the (b) panel, and 0.065 in the (c) panel. Color bars are labeled from −2σ to 2σ about the mean value of the maps, where σ indicates the standard deviation of the map.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Comparison between the spectroscopic indices based on the measurement methods in this paper and in A. Gonneau et al. (2016, G16). The H-band spectrum of the carbon star SHV 0536139-701604 (black) is used as an example. The spectral ranges for the DIP153 feature and its pseudocontinuum defined in G16 are marked by magenta and green colors in the upper panel. Their mean values, as indicated by the horizontal lines, are inserted to Equation (1), yielding a spectroscopic index of −0.04, literally indicating emission. In this paper, the global continuum curve (yellow in the upper panel) is used to determine the normalized spectrum (lower panel), from which the median value of the spectral range denoted by red color results in a spectroscopic index of 0.14; the positive index properly represents an absorption feature. See Figure 6 for details.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Top: J-band spectra at the central pixel in the Gemini-NIFS spectro-imaging data (black). A least-squares third-degree polynomial fit used to define the continuum flux density (yellow). The area masked in gray is not used in the continuum fitting. In the 1.275–1.290 μm range, an artifact remains after telluric correction. The yellow bar plotted on the bottom left shows the residual standard error of the fit, mostly attributed to weaker spectral features that are not considered in this paper. Bottom: spectrum normalized by the continuum as a result of the polynomial fit. The yellow bar on the left presents the uncertainty propagated from continuum fitting.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Three combinations for magnitude difference between the JHK-band images: (a) (J − H), (b) (H − K), and (b) (J − K) color maps. The redder color of the maps toward the center indicates the intrinsically red nature of the central star. Black contours display the corresponding 0.8 μm brightness distribution (see Figure 2 for details).
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Same as Figure 5 but for H-band spectra at the central pixel. The 1.53 μm absorption feature (DIP153; 1.50–1.59 μm), marked in red, is prominent. The median of the normalized spectrum is 0.85, corresponding to a spectroscopic index of 0.18 (see text). The COH52 (1.5974–1.6026 μm), COH63 (1.6174–1.6226 μm), and C2 (1.7680–1.7909 μm) absorption features are marked in blue.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Same as Figure 5 but for K-band spectra at the central pixel. The CO12 (2.2931–2.2983 μm) absorption feature is marked in red, and the median value of its normalized spectrum is indicated as 0.94. The CaI (2.255–2.265 μm) and CO13 (2.3436–2.3488 μm) absorption features are marked in blue.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Reproduction of the spectroscopic indices following the method defined in A. Gonneau et al. (2016). See Figure 8 for details, except for vertical bars indicating uncertainties propagated from the fluctuation in the relevant pseudocontinuum band pass.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: A new index DIP153b defined by A. Gonneau et al. (2017, G17) through an empirical fitting for the DIP153 index used in A. Gonneau et al. (2016), locating open circles in the left panel near the zero level. For the right panel, the same formula is applied to the DIP153 index used in this paper based on the continuum fitting over the H band. See Figures 8 and 12 for details.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Time residuals of exoplanets in Sections 4.2 and 4.3
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Inspiral Timescale for exoplanets in our sample. Gray: exoplanets with mass M ≲ 0.25MJ; Black: HJ (0.25MJ < M ≲ 13.6MJ). The stellar ages are taken from: A. Pál et al. (2010); T. Chan et al. (2011); G. Á. Bakos et al. (2010); J. D. Hartman et al. (2009); A. W. Howard et al. (2012); J. D. Hartman et al. (2011a); D. M. Kipping et al. (2010); J. D. Hartman et al. (2011b,2011c); B. Sato et al. (2012); J. D. Hartman et al. (2012); T. G. Ellis et al. (2021); A. Bieryla et al. (2015); L. Ghezzi et al. (2018); A. S. Bonomo et al. (2017); R. Petrucci et al. (2013); M. Gillon et al. (2009a); D. R. Anderson et al. (2011); C. Hellier et al. (2009); L. Hebb et al. (2010); C. Hellier et al. (2010); F. Faedi et al. (2011); G. Scandariato et al. (2022); C. Hellier et al. (2012); D. R. Anderson et al. (2014); R. G. West et al. (2016); B. Smalley et al. (2012); A. H. M. J. Triaud et al. (2013); C. D. McGruder et al. (2023); C. Hellier et al. (2014); L. Delrez et al. (2016); K. W. F. Lam et al. (2017); R. Rodrìguez Martìnez et al. (2020).
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Time residuals from TTV fitting, LOOCV analysis, and corresponding ΔBIC of exoplanets studied in Section 4.1. For each exoplanet: Top panel: time residual results using 5σ rejection scheme. The second panel: time residual results using 3σ rejection scheme. The blue curves and shaded areas indicate the best-fit quadratic model. Orange points are based on previous literature data. Green points are based on TESS data. Red points are based on HST data from this work. Gray points are clipped data. The third panel shows the period change rate dp/dt from fitting a quadratic model after removing each transit timing data point. Orange squares indicate dp/dt values 3σ away from zero, while purple diamonds represent values within 3σ. The dashed–dotted line marks the original dp/dt fit, with the green shaded area showing the 1σ confidence region. The bottom panel displays the corresponding ΔBIC.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Timing residuals when conducting the TTV modeling of WASP-12 b. Top panel: quadratic fitting of the HST data alone. Bottom panel: quadratic fitting of the HST and TESS data together. We obtain ﹩\dot{P}=-31.36\pm 2.95﹩ ms yr−1 when fitting the HST data alone, and ﹩\dot{P}=-32.84\pm 1.78﹩ ms yr−1 when fitting the HST and TESS data together. For comparison, the original fitting in Section 3.2 with all selected archival data yields ﹩\dot{P}=-30.31\pm 0.85﹩ ms yr−1.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Quadratic TTV model fitting results of all exoplanets in our sample that show an orbital period variation trend consistent with a constant period.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: (Continued) Quadratic TTV model fitting results of all exoplanets in our sample that show an orbital period variation trend consistent with a constant period.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: While jointly fitting HD 206893 B and c’s orbits, we find an insensitivity to the mass of B. To illustrate this effect, we select the MEGNO plots for MB = 17.0 MJup and MB = 37.0 MJup using the orbital parameter determinations from both Efit5 and orbitize! after letting the planets orbit for 1 Myr. For any chosen value of the mass of B, the most stable systems require an orbital eccentricity of B of ∼0.14 and a low value of eccentricity for c of <0.2 with the most stable orbits at ec ∼ 0.1.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Top: Sampled orbital fitting of HD 206893 B including astrometry from S. Hinkley et al. (2023) and RV measurements from KPIC in 2020 and 2022 using observable-based priors. Orbits are shown in gray, with the astrometry measurements in blue. Bottom: the RVs of each gray orbit are plotted with KPIC RV measurements.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: We investigate the stability of HD 206893 B for the retrieved age of the system, 144 Myr. We observe that there are islands of stability, favoring lower eccentricity. Like our mass estimates from evolutionary modeling, we find that 22 MJup mass and 30 MJup mass objects appear to have the highest percentages of stable orbits over the life of the system, with the most stable configuration being a 35 MJup companion on a perfectly circular orbit.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: The “survivability” of coplanar vs. noncoplanar systems. When HD 206893 B and c are coplanar, we see a higher maximum percentage of stable systems after 1 Myr with a lower value of ec and higher value of eB at 0.1 < eB < 0.2.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Same as Figure 16, but only fitting using K-band data.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: Combined grating data from all 11 Chandra/ACIS/HETG observations of HL Tau, with spectral lines of interest labeled. The best-fit model fit jointly to the individual zeroth-order and combined grating spectra is shown in orange. Left inset: a zoom-in on the region around the Fe XXV feature at 1.85 Å (6.7 keV) shows a clear detection of the Fe XXV line and a marginal detection of the 6.4 keV neutral Fe fluorescence line in ∼300 ks. Right inset: a zoom-in on the 6–7 Å region shows a strong detection of the f line of the Si XIII He-like triplet and a fainter but still present detection of the r line. Inset units are same as in the larger figure.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: Comparison of model fits to HL Tau observations from 2000 to 2020. All models use one APEC plasma component with variable temperature and a fixed abundance for Fe (and elements with Fe-like FIP) set at the best-fit value from a joint fit to the faint XMM-Newton observations from 2020 and a variable absorption component. Top row: flux is shown both absorbed (as observed; blue for XMM-Newton, green for Chandra) and unabsorbed (corrected for NH; brown). Second row: the plasma temperature for the single plasma component (red) in comparison to 4 keV. Third row: the emission measure for the single plasma component (red). Bottom row: the column density NH of the absorbing material (black). Observing windows are labeled above each column. The observations during the flare identified by G. Giardino et al. (2006) in 2004 are highlighted in gray.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: Lomb–Scargle periodograms of the high-energy light curves for HL Tau from the XMM-Newton MOS1 (solid blue), MOS2 (solid orange), and PN (solid green) detectors and all three jointly (black). The Lomb–Scargle periodograms of the window functions (i.e., flat data with identical timing and uncertainties to the observed data) for the three detectors are depicted as fainter dotted lines with the same colors as those derived from data. The strongest peak of the data is at a minimum of the periodogram of the window function, indicating that this is not due solely to the observing window. The strongest peak of the window function, at ∼2 days, corresponds to XMM-Newton’s orbital period.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: X-ray images of HL Tau from XMM-Newton EPIC observation 0109060301. The MOS2 image (middle panel) shows contamination of the core of the HL Tau (right source) from the wing of the PSF of XZ Tau AB (left source). This does not occur for the MOS1 (top panel) or PN (bottom panel) detectors. Cyan contours depict the extraction region for HL Tau (circle) and the background (partial annulus around XZ Tau).
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: The high-energy (>2 keV) XMM/PN light curve of HL Tau from 2020, in chronological order (left) and phased to a ∼21-day period (right). Colors distinguish data from each observation and are the same for each observation in both panels. Count rates are derived from binning by 1 ks.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: Temperature vs. unabsorbed X-ray luminosity for single-temperature fits to HL Tau (green crosses), in comparison to temperature and unabsorbed luminosities from two-temperature fits (blue and orange circles) to the COUP pre-main-sequence stars (T. Preibisch et al. 2005).
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: Left: the zeroth-order light curve from the 2018 Chandra observations. Right: the Lomb–Scargle periodogram for these data (solid) and its window function (dotted). The strong peak in the window function near 2.5 days is consistent with the orbital period of Chandra.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: The low-energy (<2 keV) XMM-Newton EPIC/PN light curve of HL Tau. Soft count rates are typically <35% of simultaneous hard count rates, due to the plasma temperature and high absorption.