adsabs/AstroCLIMB huggingface dataset:
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 11, but for Architecture IIb.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 10, but for Architecture IIa.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 9, but for Architecture IIb.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 11, but for Architecture V.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 10, but for Architecture V.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 9, but for Architecture V.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 11, but for Architecture VIIIb. This includes using Equation (2) for finding the sensitivity due to the varying precision of the measurements.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 11, but for Architecture VIIIa. This includes using Equation (2) for finding the sensitivity due to the varying precision of the measurements.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 10, but for Architecture VIIIb.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 10, but for Architecture VIIIa.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 9, but for Architecture VIIIb.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 9, but for Architecture VIIIa.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 10, but for Architecture VI.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 9, but for Architecture VI.
Paper: Simulations for Planning Next-generation Exoplanet Radial Velocity Surveys
Authors: Patrick D Newman, Peter Plavchan, Jennifer A. Burt, Johanna Teske, Eric E. Mamajek, Stephanie Leifer, B. Scott Gaudi, Gary Blackwood, Rhonda Morgan
Figure caption: Same as Figure 11, but for Architecture VI.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: The detection limit for Altair—the dashed line is the lower limit and the dotted–dashed line is the upper limit. The star points correspond to all the discovered candidates, during all the surveys (including the NIRI, NACO, ADONIS, and PUEO data). The detection limit was calculated from the NIRI data, assuming that the VLT was similar. The two lines correspond to the lowest and highest detection limits. This varies significantly, due to the conditions during the different observing nights. All discoveries fall under the lowest detection limit (the dashed line).
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Galactic distribution of the target sample. Top: the number of companions for each sample star. Bottom: distinction between the stars for which all detections are (very) likely companions (pluses) and those for which a number of detections have been rejected, i.e., with more detections than (very) likely companions (squares). Note: sample stars with detections but no companions appear as squares in the lower panel, while stars without any detections are not plotted.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Brightness distribution of the stars within 30′ of HD 101412. The potential companion that was detected near HD 101412 has a magnitude K = 14.466. To determine the surface density for stars with K ≥ 14.466, the distribution was extrapolated out to K = 18, using a polynomial fit.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Angular separation vs. ΔK for all detections. The squares are the “very likely” physical companions; the triangles are the “likely” companions; and the small circles are “unlikely” to be companions. See the text for the definitions.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Distribution of the sample by spectral type and distance. The second bar, labeled “Be,” shows B-type stars of uncertain spectral type, while the last bar is for a continuum star. Further details are given in Section 2.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: The effect of cloud decks on GJ 486b’s spectrum. Top left: GJ 486b model spectra of a hydrogen-dominated atmosphere with water at solar abundances. The pressure of the cloud deck, P  c , is indicated in the legend as ﹩{\mathrm{log}}_{10}(﹩                   P  c ) and corresponds to a range of 10-6–10−2 bar. Top right: The same model spectra as in the top left, except the continuum has been subtracted. Lower left: Auto-cross-correlation functions for the models shown in the top row. Lower right: Auto-cross-correlation peak amplitude.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: Simulated JWST transmission spectra for possible GJ 486b atmospheric compositions allowed by our high-resolution observations. In all panels, we show the models at a resolving power of R = 2700 (light blue), corresponding to the native resolution of NIRSpec/G395H, as well as the models binned to a resolution of R = 100 (navy lines). The top four panels show models with variable H2O abundances and mean molecular weights with CO2 fixed to a solar abundance. The lower four panels switch the roles of CO2 and H2O.
Paper: High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b
Authors: Andrew Ridden-Harper, Stevanus K. Nugroho, Laura Flagg, Ray Jayawardhana, Jake D. Turner, Ernst de Mooij, Ryan MacDonald, Emily Deibert, Motohide Tamura, Takayuki Kotani, Teruyuki Hirano, Masayuki Kuzuhara, Masashi Omiya, Nobuhiko Kusakabe
Figure caption: The significance to which injected cloud-free solar abundance models are recovered from our data as a function of temperature for GJ 486b. These models were generated by GGchem and used different approaches for modeling the effect of condensation on the abundance profiles. However, the transmission spectra resulting from these models do not account for clouds or haze that may form from this condensation. The blue solid line did not account for condensation, the orange dashed line did account for condensation, and the green dotted line accounted for condensation but condensates were removed to model rain out.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Distributions of the basic properties of the cloud, including peak intensity, projected angular area, velocity dispersion of average spectrum, and flux. The colors represent different isotopologues. Each point is the value of the probability density function at the bin, normalized such that the integral over the range is 1. Without bins with unity width, the histogram values will not sum up to 1. The solid lines fit the power-law distributions of basic properties, with the formula dN/dX ∝ X−(α+1). The results of index α are shown in the figures with errors, but the error of ﹩{T}_{\mathrm{peak}}^{18}﹩ cannot be calculated because of poor pixel number and distribution region.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Statistical comparison of flux and pixel number of 13CO emission using different algorithms. The dotted line is the region where y = x. The number in the figure represents the number of signals that can be detected by both algorithms. The units of flux are K km s−1 arcmin2.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The spatial distribution of C18O emission in cloud G207.017−01.825+015.40 (known as the Rosette Nebula; Li et al. 2018) based on different algorithms. The background is the 12CO intensity, and the contour shows the boundary of C18O emission.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The spatial distribution of 13CO emission in cloud G207.017−01.825+015.40 (known as the Rosette Nebula; Li et al. 2018) based on different algorithms. The background is the 12CO intensity, and the contour shows the boundary of 13CO emission.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Statistical comparison of flux and pixel number of C18O emission using different algorithms. The dotted line is the region where y = x. The number in the figure represents the number of signals that can be detected by both algorithms. The units of flux are K km s−1 arcmin2.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The spatial distribution of C18O emission in cloud G217.383−00.083+026.19 (known as Sh 2–287; Gong et al. 2016) based on different algorithms. The background is the 12CO intensity, and the contour shows the boundary of C18O emission.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The spatial distribution of 13CO emission in cloud G217.383−00.083+026.19 (known as Sh 2–287; Gong et al. 2016) based on different algorithms. The background is the 12CO intensity, and the contour shows the boundary of 13CO emission.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The peak velocity distribution of the clouds. The y-axis is the cloud number to find a peak velocity of a cloud within 4 km s−1 around the bin center, which is marked with circles, inverted triangles, and squares for the 12CO, 13CO, and C18O emission, respectively.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:  13CO and C18O percentage rates pixel by pixel against different spectral parameters (peak intensity, integrated intensity).
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Proper-motion graphs, part 1. The legend is as follows: • = 2005 Survey (or 1995 Survey, if there are no data from the 2005 Survey); ♦ = 1995 Survey; △ = Pirzkal et al. (1997); ▽ = Leinert et al. (1997); ▷ = Perrin (2006); □ = Ageorges et al. (1997); x = Correia et al. (2006); ⋆ = Ghez et al. (1997); ◦ = Cohen et al. (1985), Koresko et al. (1991), Bernacca et al. (1993), Reipurth & Zinnecker (1993), Perez et al. (2004), Smith et al. (2005), Vink et al. (2005), Lafrenière et al. (2008), Turner et al. (2008), and Uyama et al. (2017), depending on the system.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Examples of a common proper-motion star (left) and a potential background star that remains inconclusive (right). Indeed, on the right graph, the error bars are such that the candidate could either be a background star or a common proper-motion star. The legends are as follows. For HD 97300: • = 2005 Survey; ▷ = Perrin (2006); and ◦ = Lafrenière et al. (2008). For MWC 297: • = 2005 Survey; ⋆ = Ghez et al. (1997); and ◦ = Vink et al. (2005).
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Companion sample by distance and linear separation. Left: the companions found around 45 cool stars (≤12,500 K). Right: the companions found around 16 hot stars (>12,500 K). The dashed lines indicate the detection limits, as discussed in the text.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Proper-motion graphs, part 3. The legend is as follows: • = 2005 Survey (or 1995 Survey, if there are no data from the 2005 Survey); ♦ = 1995 Survey; △ = Pirzkal et al. (1997); ▽ = Leinert et al. (1997); ▷ = Perrin (2006); □ = Ageorges et al. (1997); x = Correia et al. (2006); ⋆ = Ghez et al. (1997); ◦ = Cohen et al. (1985), Koresko et al. (1991), Bernacca et al. (1993), Reipurth & Zinnecker (1993), Perez et al. (2004), Smith et al. (2005), Vink et al. (2005), Lafrenière et al. (2008), Turner et al. (2008), and Uyama et al. (2017), depending on the system.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Proper-motion graphs, part 4. The legend is as follows: • = Th07 (or the B95 Survey, if there are no data from Th07); ♦ = B95; △ = Pir97; ▽ = Lei97; ▷ = MP06; ⋄ = Cohen85; □ = Ageorges97; x = Correia06; ⋄ = Cohen85; and ⋆ = Ghez97.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Companions as a function of primary effective temperature. Top: ΔK relative to the primary star. Bottom: linear separation. The symbols distinguish binary, triple, and higher-order multiple systems, while the shading indicates the very likely (black) and the likely (gray) companions. Note: there are two triangles per primary star, and the 17 diamond symbols are associated with four systems at 7200, 10,500, 22,000, and 31,000 K.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Linear separation and ΔK of all the companions. The symbols are as in Figure 11; the dashed lines indicate the detection limits, as discussed in the text.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Proper-motion graphs, part 2. The legend is as follows: • = 2005 Survey (or 1995 Survey, if there are no data from the 2005 Survey); ♦ = 1995 Survey; △ = Pirzkal et al. (1997); ▽ = Leinert et al. (1997); ▷ = Perrin (2006); □ = Ageorges et al. (1997); x = Correia et al. (2006); ⋆ = Ghez et al. (1997); ◦ = Cohen et al. (1985), Koresko et al. (1991), Bernacca et al. (1993), Reipurth & Zinnecker (1993), Perez et al. (2004), Smith et al. (2005), Vink et al. (2005), Lafrenière et al. (2008), Turner et al. (2008), and Uyama et al. (2017), depending on the system.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Comparison of the statistical (squares, triangles, and crosses) and proper-motion (circles) results for all the detections that are common to both studies. The symbols without circles have inconclusive proper-motion results, while the dotted circles indicate that the common proper-motion results are questionable.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Proper-motion graphs for the targets for which our statistical and proper-motion studies do not match. The legend is as given in Table 7.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Multiplicity plotted by effective temperature and distance for the HAEBE Sample.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: The probability of detecting a companion as a function of separation and magnitude difference.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Examples of detections: HBC 334, HD 37411, HK Ori, and XY Per. HBC 334 and HD 37411 are apparent triple systems. The orientation in each image is north to the top, east to the left.
Paper: A Survey of Herbig Ae/Be Multiplicity
Authors: S. J. Thomas, B. Rodgers, N. S. van der Bliek, G. Doppmann, J. Bouvier, C. Araya Salvo, J.-L. Beuzit, F. Rigaut
Figure caption: Multiplicity as a function of spectral type for the 126 HAEBE primary stars.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the 731 sources detected in the BJ083 and UD001 sessions, color coded to highlight the number of sessions from which successful images were produced for each source. Source decls. range between 90° and −45°, limited by the southernmost reach of the VLBA.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the source compactness ratios and their variability for the sources imaged in the BJ083 and UD001 sessions. Top panel: (a) distribution of the peak fraction, C 1, (b) the core fraction, C 2, and (c) the correlated flux fraction, C 3, taken from the last epoch that each source was observed at. Bottom panel: (d) distribution of the per-source standard deviations of the peak fraction, ﹩{\sigma }_{{C}_{1}}﹩, and (e) the core fraction, ﹩{\sigma }_{{C}_{2}}﹩, and (f) the correlated flux fraction, ﹩{\sigma }_{{C}_{3}}﹩, for the sources observed at more than one epoch. The mean and median values are given in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the flux-density-weighted radial extent and its variability for the sources imaged in the BJ083 and UD001 sessions. Top panel: (a) distribution of the flux-density-weighted radial extent, E, and (b) the flux-density-weighted radial extent within 4 mas, E 4, taken from the last epoch that each of the sources was observed at. Bottom panel: (c) distribution of the per-source standard deviations of the flux-density-weighted radial extent, ﹩{\sigma }_{E}﹩, and (d) the flux-density-weighted radial extent within 4 mas, ﹩{\sigma }_{{E}_{4}}﹩, for sources observed in more than one epoch. The mean and median values are given in the top-right corner.
Paper: The Celestial Reference Frame at K Band: Imaging. I. The First 28 Epochs
Authors: Aletha de Witt, Christopher S. Jacobs, David Gordon, Michael Bietenholz, Marisa Nickola, Alessandra Bertarini
Figure caption: Distribution of the radial extent and its variability for the sources imaged in the BJ083 and UD001 sessions. Top panel: (a) distribution of the radial extent, R, and (b) the radial extent within 4 mas, R 4, taken from the last epoch that each of the sources was observed at. Bottom panel: (c) distribution of the per-source standard deviations of the radial extent, ﹩{\sigma }_{{R}_{4}}﹩, and (d) the radial extent within 4 mas, ﹩{\sigma }_{{R}_{4}}﹩, for sources observed in more than one epoch. The mean and median values are given in the top-right corner.