adsabs/AstroCLIMB huggingface dataset:
Paper: High Proper Motion Discoveries from the UKIRT Hemisphere Survey
Authors: Wings Zhang, Adam C. Schneider, Thomas P. Bickle, Adam J. Burgasser, Emma Softich, Federico Marocco, Daniella Bardalez Gagliuffi, Jacqueline K. Faherty, Aaron M. Meisner, J. Davy Kirkpatrick, Marc J. Kuchner, Martin Kabatnik, Frank Kiwy, Arttu Sainio, Jörg Schümann, Karl Selg-Mann, Nikolaj Stevnbak Andersen, Bruce Baller, Paul Beaulieu, John Bell, Dan Caselden, Guillaume Colin, Alexandru Dereveanco, Christoph Frank, Konstantin Glebov, Léopold Gramaize, Leslie K. Hamlet, David W. Martin, William Pendrill, Stéphane Perlin, Andres Stenner, Christopher Tanner, Melina Thévenot, Vinod Thakur
Figure caption: Histogram of total proper motion values for new discoveries in this work.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Spatial and proper motion distribution of cluster members for [1] Cluster 123 and [2] Cluster 163. (a) The subplots display YSO cluster members overlaid on a WISE 12 μm inverse gray-scale mosaic in the R.A.–decl. plane. The white dashed–dotted circle indicates the region analyzed for cluster membership. Orange squares indicate Gaia-matched SFOG YSOs, while cyan diamonds represent Gaia-only cluster members from DR3. Red squares mark SFOG-only YSOs from E. Winston et al. (2020). Bright green squares denote SFOG-only YSOs within the 30th- and 70th percentile YSO density contours (green dashed curves) for Clusters 123 and 163, respectively, which are also included as cluster members. The YSOs, used to create the contour, are identified cluster members from the HDBSCAN-MC and GOLDFIST simulation and therefore are more evolved Gaia-only or Gaia-matched SFOG YSOs. (b) The ICRS distance distribution of cluster members is illustrated, with the blue-filled plot representing the median distance and the red dashed and black dashed–dotted lines indicating the 16th and 84th percentiles, respectively. (c) Proper motion vector plot comparing observed and simulated cluster members. The color scale represents the number density of observed members (squares) selected using the Monte Carlo threshold (﹩{ \mathcal M }{{ \mathcal C }}_{\mathrm{thr}}﹩). Observed field YSOs are shown as cyan circles. The inset highlights simulated cluster members, while gray error bars, displayed with reduced opacity, indicate proper motion uncertainties. This subplot compares the proper motions of simulated and observed cluster members.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: The Monte Carlo spectra for field and member YSOs in (a) Cluster 123 and (b) Cluster 163. The kinematic distance estimate for Cluster 123 is unknown, with the simulation predicting a distance of 740 pc ± 6 pc. For Cluster 163, the kinematic distance estimate is 9900 pc, while the simulation predicts a distance of 3531 pc ± 444 pc. The green curve illustrates the decrease in observed total cluster members with increasing threshold. The black curve represents the identified total cluster members for the simulated cluster. The blue dashed–dotted line and red curve depict the decline in simulated true members and false positives, respectively, with increasing threshold. The difference between identified total cluster members for the observed and simulated clusters is shown by the black dashed–dotted line in the residual plot. The faded gray lines represent the total identified cluster members for simulated clusters generated using an alternative set of parameters, with mean squared deviation (MSD) within 3 times the MSD of the best-fit black curve from the green plot. The yellow vertical dashed–dotted line represents the final determined Monte Carlo threshold (﹩{ \mathcal M }{{ \mathcal C }}_{\mathrm{thr}}﹩), where the simulated true members comprise 95% of the initial count. ﹩{ \mathcal M }{{ \mathcal C }}_{\mathrm{thr}}﹩ is 4000 and 6500 for Clusters 123 and 163, respectively.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Spatial distribution of cluster members in the W4/W5 complex (Cluster 257). (a) The subplot shows YSO cluster members overlaid on a WISE 12μm inverse gray-scale mosaic in the R.A.–decl. plane. The white dashed–dotted circle indicates the region analyzed for cluster membership. Orange squares mark Gaia-matched SFOG YSOs, cyan diamonds indicate Gaia-only YSOs, and red squares denote SFOG-only YSOs from E. Winston et al. (2020). SFOG-only YSOs within the 30th percentile YSO density contour (green dashed curve) are included as cluster members (bright green squares). The contour is based on HDBSCAN-MC and GOLDFIST-identified cluster members—more evolved Gaia-only or Gaia-matched SFOG YSOs. (b) The ICRS distance distribution of cluster members is illustrated. The blue-filled plot shows the median distance, with the 16th and 84th percentiles marked by red dashed and black dashed–dotted lines. This figure presents the spatial distribution of YSO cluster members in both R.A.–decl. and ICRS distance space for the W4/W5 region.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Stellar spectral energy distributions (SEDs) with magnitude on the vertical axis, illustrating characteristic trends in infrared and optical magnitudes for (a) correct and (b) false SFOG–Gaia associations. The horizontal axis, plotted on a logarithmic scale, represents the wavelengths of photometric filters in micrometers (μm). Blue data points represent Gaia DR3 optical bands (GBP, G, and GRP). Green points correspond to infrared bands, including 2MASS J, H, Ks, IRAC bands 1–4, WISE W3 and W4, and MIPS 24 μm. In panel (b), the red-circled points highlight deviations from the expected YSO magnitude trend, indicating a probable chance alignment between SFOG and Gaia DR3 (see Equation (1)). This figure demonstrates the photometric method used to identify 94 one-to-one chance alignments.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: High-level block diagram illustrating cluster simulation using multidimensional global optimization. The diagram illustrates a single iteration of the optimization process. For both spatial and proper motion optimizations, Popsize in differential evolution is fixed at 150, yielding a total population (Np) of 750 for five-parameter optimization and 150 for single-parameter optimization. The mutation factor (F) varies between 0.5 and 1.5, with the crossover probability (Pcr) set at 0.5. Both optimizations employ the “best1bin” strategy with a tolerance (tol) of 0.5. Computations are parallelized across 80 CPU cores for enhanced computational efficiency during both stages of optimization.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Example of ideal simulation for Cluster 257 [W4/W5 complex] with King model in (RA, Dec, ICRS distance) space (a) Simulated cluster with King profile. Blue points represent cluster members. There are 452 members in the simulated YSO cluster. (b) Represents the simulated cluster embedded in a uniformly distributed low-density foreground and background field YSO cone. (c) Distribution of cluster and field YSOs plotted on nearly the same scale as in (a). About 58% of the total YSOs (779) are cluster members (452), which implies model parameter Φmem = 0.58.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Proper motion vector plot for YSOs in the Taurus–Auriga complex. Red points represent 349 YSOs with Gaia counterparts exhibiting ruwe < 1.4. The color bar indicates the YSO number density, while the inset highlights 58 YSOs (green circles) selected to extrapolate proper motions for simulating cluster members.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: Average activity data vs. S-STD are plotted for four equally spaced mass bins that decrease from top to bottom. The left, middle, and right columns show, respectively, the median S-value, the ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩-N1984 value, and the ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩-LO2018 metric on the x-axis. For each panel, the Pearson correlation coefficient (P-CC) is calculated separately for the cycling stars (blue symbols) and all stars in each mass bin. We find the correlations between activity variation and each activity metric vary by mass bin, with S-value showing the strongest correlation on average. From the noncycling stars (gold symbols) we single out HD 166620 (magenta), τ Ceti (green), and HD 190067 (brown). Gray data points represent stars from all mass bins.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: Fundamental stellar properties vs. S-STD are plotted for four equally spaced mass bins that decrease from top to bottom. The left, middle, and right columns plot the Teff, ﹩{\mathrm{log}}\,(g)﹩, and [Fe/H] vs. S-STD, respectively. Gray data points represent stars from all mass bins. We find the subsolar-mass bins have more consistent P-CC values than the supersolar-mass bin for all three stellar properties. The noncycling stars behave similarly to the cycling stars, but at lower S-STD values, suggesting the inactive stars represent a stage of activity that stars reach after their cycling amplitudes are no longer detectable. A representative error bar is shown for the x-axis values. From the noncycling stars (gold symbols) we single out HD 166620 (magenta), τ Ceti (green), and HD 190067 (brown).
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: S-STD is plotted as a function of median S-value, ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩-N1984, and ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩-L02018 for stars with masses between 0.7 and 1.1 M⊙. The more active stars, with ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩ > −4.90, are in green, and the less active stars that compose our primary sample are in brown. The vertical stratification for any given value of the average activity displays the S-STD as a valuable metric for studying main-sequence magnetic field evolution.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: Stellar activity cycle period binned by stellar mass. We do not see the same tight correlation with temperature and cycle period for stars more active than ﹩{\mathrm{log}}\,({R}_{\mathrm{HK}}^{{\prime} })﹩ (N1984) of −4.90 compared to the tight correlation when binned by Teff (H. Isaacson et al. 2024). The stars less active than −4.90 have large scatter in cycle period for a variety of time-averaged activity values. Gray data points represent all mass bins.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: The cycle period vs. cycle amplitude for stars with masses between 0.7 and 1.1 M⊙. Across the subsolar-mass bins, the primary feature is a maximum in the amplitude distribution at a period of 10 yr. The correlation coefficients are strongest in the two lowest-mass bins, and nearly zero in the near-solar-mass bins. The secondary feature is that cycle periods longer than 15 yr have consistently low amplitudes. Perhaps passing the 15 yr threshold is the point of no return and cycles only tend toward longer and smaller-amplitude cycles.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: Fundamental stellar properties vs. stellar cycle periods are plotted for four mass bins. The equally spaced mass bins decrease from top to bottom. The left, middle, and right columns plot the Teff, ﹩{\mathrm{log}}\,(g)﹩, and [Fe/H] vs. cycle period, respectively. Gray data points represent stars from all mass bins. If one of the parameters was critical in determining the cycle period, we would see a strong P-CC for all mass bins, but no property shows such consistency.
Paper: The California Legacy Survey. VI. The Fate of Activity Cycles in Sun-like Stars
Authors: Howard Isaacson, Stephen R. Kane, Brad Carter, Andrew W. Howard
Figure caption: Teff, ﹩{\mathrm{log}}\,(g)﹩, and stellar mass are shown for our sample of stars. They have masses between 0.7 and 1.1 M⊙. Stars with similar masses can have a range of Teff. We narrow the ﹩{\mathrm{log}}\,(g)﹩ range to assess magnetic field changes for stars while they are still on the main sequence. Both the cycling stars and noncycling stars are plotted.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: LC fitting results for systems TIC 369605666 and 54759992, with starspots set during LC modeling. For TIC 369605666, the analysis utilized data drawn from short cadence observations within the BJD interval of 2459833–2459837. For TIC 54759992, analysis was based on data selected from Sector 43, encompassing the BJD range of 2459507–2459511.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: SED fitting of TIC 54759992 (LAMOST 0634+1852) with two components. The red dots denote the observations used for the fitting, including Gaia Data Release 2 and DR3, APASS, 2MASS, and WISE (W1 and W2) observations. The observations from PS1 in the g, r, i, z, and y bands (11.08, 10.85, 10.73, 10.73, and 10.75 mag) severely surpass the brightness limits specified for stars in these bands, as presented in Table 11 of K. C. Chambers et al. (2016). As a result, photometric data from APASS are used instead of those from PS1. The red curve represents the spectral template with parameters of Teff = 6822 K, logg = 4.3 dex, and [Fe/H] = −0.5 dex; the blue curve represents the spectral template with parameters of Teff = 5736 K, logg = 4.5 dex, and [Fe/H] = −0.5 dex. The black curve shows the composite spectral template. The residuals are calculated as (observed − calculated)/observed. The central wavelengths of several primary wave bands are indicated by gray vertical lines.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: The upper panel illustrates all the samples on an M–R diagram. The solid and dashed lines represent the zero-age main sequence (ZAMS) and terminal-age main sequence (TAMS), respectively, with color-coded [M/H] according to PARSEC. Circles indicate primary stars, while triangles represent secondary stars, and colors differentiate data from various sources. The lower panel shows the full set of samples on an ﹩M-{\mathrm{log}}\,(L/{L}_{\odot })﹩ diagram, maintaining consistency in visual elements with the upper panel.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Fitting results of LAMOST-MRS spectra (gray) for TIC 369605666 (upper) and 54759992 (lower) with 10 exposures each, using parameter sets from spectral disentangling (blue line) and WD modeling (red line). The displayed wavelength range (5150–5220 Å) highlights the fit to the main absorption Mg b triplet. Additional details align with the caption in Figure 3.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: M–R diagrams for the samples are presented. Panels (a)–(c) display samples with metallicities of around −0.5, −0.25, and 0, respectively, within the M–R context. The PARSEC version 1.2s isochrones are drawn, calculated for metallicities of [M/H] = −0.5, −0.25, and 0, respectively, covering ages from 1 to 10 Gyr.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Corner plot of SED fitting results for TIC 189069314 and 54759992. The parameter values are the median of the 1D distributions, indicated by the red solid lines, while the vertical dashed lines are located at the 16th and 84th percentiles.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: LCs and spectroscopic orbit models for the remaining samples are presented, with the layout and all data markers (plot symbols) consistent with those in Figure 1.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Consistent with the content shown in Figure 10, this presents the other four systems. For eccentric binary systems, the RVs are phase folded with respect to the time of periastron passage.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Corner plot of SED fitting results for the remaining samples. The parameter values are the medians of the 1D distributions, while the vertical dashed lines are located at the 16th and 84th percentiles.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: In-line with the content illustrated in Figure 12, this displays the other four samples.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: For the case close to the projected edge of the Cygnus Rift, four examples showing an anticorrelation between extinction and integrated CO intensity in dense regions, which can also serve as strong evidence for determining distances. Here, the greyscale image represents the integrated intensity of MWISP 12CO. Similarly, thin red contours indicate the cumulative values of the extinction within the corresponding distance interval. Blue contours denote local minima of extinction (identified using minimum_filter in Scipy.ndimage) that coincide with dense gas regions (≳20 K km s−1). The distance interval, velocity interval, and determined distances are annotated at the top of the figure.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: Relations between Sdiff and Aλ dispersion σ, number density n, and slope k. (a) Set n = 0.1 pc−1 and k = 0.003 mag · pc−1, ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}\propto \sigma ﹩ when σ becomes larger. (b) ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}\propto \sqrt{n}﹩. (c) Set σ = 1 mag, the relation between ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}﹩ and k shows a similar trend to panel (a). Panel (d) is a zoom-in from panel (c).
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: The blue dots are preset to indicate jump points at two locations, 400 pc and 1500 pc, while the green dots are preset to indicate a jump point at 800 pc. In panel (a), C is set to 2, and in panel (b), C is set to 3, with 4 and 2 jump points detected, respectively.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: An example for simple one-jump-point case, denoting the relationship between ﹩{{{\rm{S}}}}_{{{\rm{diff}}}}^{{{\rm{Avg}}}}﹩, ΔAG, σ, and n. (a) Set stars number N = 1000, ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}\propto \sigma ﹩ when σ ≳ ΔA. (b) N = 1000, ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}\propto {{\rm{\Delta }}}A﹩ when ΔA ≫ σ. (c) ﹩{S}_{{{\rm{diff}}}}^{{{\rm{avg}}}}\propto \sqrt{n}﹩. The zoom-in area is presented for comparable ΔAG and σ.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: Four examples for G079.87+01.17, G074.56+00.84, G012.68-00.18, and G209.00-19.38. Stars are represented by gray dots, while black dots denote binned points every 20 pc. All four examples corresponding to the masers are located at the last jump point.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: The D–S plot in the presence of a slope in D–A space. Six false change points are noted by red crosses (I, II, III, IV, V, VI are the serial numbers of the detection in iterations). The curve is best fit by using the least squares method (in green). In comparison, a predicted parabola curve (in blue) is drawn using our preset parameters. The colored curves are the D–S of shuffled samples.
Paper: A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916’s Dust Morphology
Authors: Jamie R. Lomax, Emily M. Levesque, John P. Wisniewski, John H. Debes
Figure caption: HST/STIS BAR5 imagery of CD -31°4916’s circumstellar material. Regions with no data or that are behind masks that we created for the occulter and diffraction spikes are white in color. The relative surface brightness of the circumstellar material is shown on the same scale for both images. Crosses mark the location of the system’s central star. The white contours are equally spaced in surface brightness and are marked on the same scale for both images. The contours show the asymmetry of CD -31°4916’s surrounding dust, which is most easily seen in the east–west direction. In particular, material of the same surface brightness is farther from the star toward west side than the east side. Left: Final median combined imagery using diffraction spike masks that cross like an “X” at the center. Right: Final median combined image using diffraction spike masks that do not cross at the center.