adsabs/AstroCLIMB huggingface dataset:
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Diagnostic diagram for the coldest water detected at MIRI wavelengths, using the temperature-dependent flux ratio between the two low-energy lines near 23.85 μm illustrated in three examples in the top-right inset (for their properties, see Table 1). Slab models in LTE are shown with gray lines over a range of column densities between 1016 cm−2 (giving optically thin emission) and 1019 cm−2 (giving optically thick emission), as shown in the legend. The sample analyzed in this work is distributed using to the measured line flux ratios along the 1017 cm−2 model, assuming it as an average column for the cold reservoir. The range of snowline temperatures from K. Lodders (2003) is shown for reference. The plot to the right shows that disks with larger 1500/6000 K ratio also have larger asymmetry in the 23.85 μm lines, indicative of prominent colder water.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Demonstration of line selection for definitions of line ratios used in Figure 10, showing line fluxes (top) and the rotation diagram (bottom) as a function of the upper-level energy of individual water transitions. The very different spectral line flux distribution of the hot-dominated CI Tau and cool-dominated GQ Lup shown in Figure 8, here shown as a function of Eu, is once again very visible. Gray data points are all lines used in this work (Appendix C), colored data points are the lines at 14–18 μm explained in Section 3.2 plus the two lower-energy lines near 23.85 μm. The line ratios at 1500, 3600, and 6000 K reflect the relative flux at different temperatures. The line ratio at 3340 K between two lines with very different Aul (shown proportional to the symbol size) reflects the optical depth. Rotation diagrams for the whole sample are shown in Figure 27 in Appendix G.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Representative water spectra for a hot-dominated (CI Tau) and cool-dominated (GQ Lup) disk are shown in comparison to temperature component models (bottom). The different spectral line flux distribution is very visible, with the strongest lines having similar flux across MIRI wavelengths in the case of a hot-dominated spectrum vs. increasingly stronger lines at longer wavelengths when emission from cooler water is present. The full sample is shown in Appendix H. The H2 transition near 17 μm is marked with a green dashed line.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Trends between the water lines from Table 1 and the accretion luminosity (top) or disk inclination (bottom). Linear fits and their 95% confidence intervals are shown as dashed lines and shaded regions, and their parameters are reported in Appendix E. The color coding follows that of Figure 10.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Portion of Figure 3 illustrating the effect of mutual line opacity saturation. The iSLAT hot water model from Figure 3 is now shown in light blue, and a new model with the same parameters but including line opacity overlap is shown in bold blue (using spectools_ir; C. Salyk 2022). Accounting for line saturation correctly reproduces the reduced emission from the ortho-para line pairs, but the v = 1–1 lines are still overpredicted because both models assume LTE (compare to Figure 6).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Measured line flux ratios of a v = 1–0 and a v = 1–1 line with a v = 0–0 line (see Section 3.1.4). All lines from the v = 1 level are significantly weaker than what they should be in LTE, as found previously from ground-based spectra (A. Banzatti et al. 2023b). The red lines with labeled fractions mark suppression factors in reference to a median LTE prediction (models and sample symbols are the same as used in Section 4). In the case of nondetections, 2σ limits are marked with arrows.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 5, but here illustrating the effect of non-LTE excitation. The iSLAT model is shown in light blue, and the same model with the v = 1–1 lines divided by a factor of 2 is shown in bold blue.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Radial profiles of water lines observed in CI Tau (large, multi-gapped disk dominated by a single hot water component) and GQ Lup (compact disk with strong warm and cold water components), by applying the simple Doppler mapping technique described in Section 5.3 and Figure 19. ALMA continuum images are shown for reference in each panel (F. Long et al. 2019, 2025, private communication). All lines are partially resolved in both disks, enabling estimates of emitting radii from the deconvolved line broadening. Water rotational transitions are shown as filled circles with size proportional to the line flux (to illustrate the different spectral line flux distribution as in the top panel of Figure 9), rovibrational lines with gray crosses. A power-law fit to water transitions where Doppler broadening is detected is shown with a dashed line and shaded area (95% confidence region). The best-fit slope is reported in each plot. Keplerian radii for CO and OH lines measured in this work (Figure 16 and Appendix C) are included for comparison to the water lines.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Evidence for disk-rotation Doppler broadening of molecular lines observed with MIRI-MRS. Here, we exclude disks with inner dust cavities or lower S/N (see Appendices A and H). The observed line FWHM of H2O, OH, and CO correlates with disk inclination (top) and with the high-resolution CO FWHM from ground-based observations where available (bottom). The nominal MIRI resolving power is reported as a horizontal dotted line for reference in each panel from K. M. Pontoppidan et al. (2024). The direction indicated with an arrow shows the effect of blueshifted wind absorption observed in IQ Tau (Section 5.2). Linear fits and their 95% confidence intervals are shown as dashed lines and shaded regions, and their parameters are reported in Appendix E. The color coding follows that of model series in Figure 10, as in Figure 12.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: MIRI-MRS resolving power from line width measurements in this work, as compared to recent works (I. Argyriou et al. 2023; K. M. Pontoppidan et al. 2024; gray dashed and solid lines, respectively). The unresolved H2 lines (0–0 S(1) and S(3), light-green crosses) provide useful anchor points suggesting a slightly better resolving power near 17 μm (see also Figure 15) than what was estimated in K. M. Pontoppidan et al. (2024). The absorption lines in IQ Tau (light-red open data points) demonstrate that the resolving power at the shortest wavelengths is consistent with what was estimated in I. Argyriou et al. (2023). The resolving power we adopt in this work is shown with a red dashed line (see Table 11 in Appendix F; see also K. M. Pontoppidan et al. 2024).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Left: ratios of Keplerian radii estimated from the deconvolved line widths (Figure 20) as a function of their line flux ratio, using the 1500 and 6000 K lines from Table 1. Shown here are only disks where Doppler broadening is detected (Appendix G). With the exception of IQ Tau (the disk where wind absorption is detected; see Figure 18), the trend here shows that a larger flux in the 1500 K lines corresponds to their emission coming from larger radii. Middle: illustration of the temperature gradient approximated by the three temperature regions at increasing disk radii, in reference to processes of icy pebble drift, sublimation, and gas diffusion (modified from A. Banzatti et al. 2023a). Right: summary of differences between disks that have efficient pebble traps vs. drift, based on the results from this work (see Section 6; C. E. Romero-Mirza et al. 2024a).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Evidence for Doppler broadening of MIRI water lines as a function of upper-level energy Eu. Shown are the same two disks that have a minimal warm-water component (CI Tau) vs. a strong cold water component (GQ Lup) as defined in Section 4; the rest of the sample is included in Figure 26 in Appendix G. In the upper panel, their spectra are scaled as in A. Banzatti et al. (2023a) and show individual transitions as in Figure 3. The water lines in GQ Lup become narrower at lower Eu, as expected if the cold water reservoir is in a disk region at larger radii (A. Banzatti et al. 2023a; C. E. Romero-Mirza et al. 2024a). Light-red dots show the updated MIRI resolving power at each line wavelength from Figure 16. The two lines near 1500 K from Table 1 are excluded from the fit, due to the lower resolving power at 23 μm.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Correlations between the line ratios defined in Section 4 and the dust disk size as measured from ALMA continuum images. Colored larger data points (used for the linear fit) show disks with single stars, no millimeter cavity, and no cloud contamination (see Section 4.3). The rest of the sample is shown with small gray dots and is excluded from the fit. The first two anticorrelations to the left expand what was found in A. Banzatti et al. (2023a) in four disks. Linear fits and their 95% confidence intervals are shown as dashed lines and shaded regions; their parameters are reported in Appendix E.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Absorption spectra of rovibrational CO (top) and H2O lines (bottom) in the high-inclination disk of IQ Tau. Two models with different RV, temperature, and FWHM are shown in the figure to approximately reproduce the data. The MRS data is shown in black, and the difference of the two models in red. Individual water transitions are color coded as in Figure 1, to illustrate that absorption is prevalent in lower-energy lines (cyan).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Evidence for disk-rotation Doppler broadening of molecular lines observed with MIRI-MRS. High-resolution (R > 50,000) rovibrational CO line profiles are shown in black (from J. M. Brown et al. 2013; A. Banzatti et al. 2022). The single (unblended) MIRI water line at 17.35766 μm (Eu ∼ 2400 K; Appendix C) is shown in red. A Gaussian broadening that assumes a resolving power equivalent to FWHM = 95 km s−1 is shown for comparison as a gray shaded area. The orange dashed line in IQ Tau shows the centroid of the blueshifted absorption component found in the rovibrational lines in its MIRI spectrum (Figure 18).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Keplerian interpretation for the Doppler broadening of emission lines in MIRI spectra. Line widths from Keplerian models at 0.2 au (with FWHM = 2VKepl) are shown with solid lines for a range of stellar masses between 0.25 and 1 M⊙. Their convolution to the MIRI resolving power is shown with dashed lines. For illustration, we show a selection of disks spanning the whole range in disk inclinations included in this work, and we use the 6000 K line from Table 1. The H2 line at 17.035 μm is included as a reference for the MIRI resolving power (see Figure 16).
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: The outliers deviating from the median Me values in Figure 6. The horizontal axis represents the sum of the extinction and distance modulus of the clusters, while the vertical axis indicates the deviation between the maximum Me of OC BSS and the median Me values in Figure 6. The color represents the logarithmic age of the clusters.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Panel (a) shows the core member stars in Galactic coordinates. Panel (b) presents the density profile along with the corresponding King model fitting, highlighting the boundary radius Rb. Panel (c) depicts the H-R diagram and includes the best isochrone fitting. As described in Section 4, the boxes represent the candidates for BSS: the blue boxes indicate R_BSS, while the light blue boxes indicate P_BSS; along with the positions of various star types on the H-R diagram. Gray dots indicate stars with a membership probability greater than 50%.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Continued to Figure A1.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Positional precision: residuals (ordinate) vs. ρ (abscissa). Differences between the measured ρ in the radial and tangent direction, Δρ, ﹩\overline{\rho }\cdot {\rm{\Delta }}\theta ﹩, both in mas and in position angle Δθ (in degrees), as a function of the mean ρ at a given epoch, for all the objects in our sample that have simultaneous observations in both filters. The first two rows of panels show the residuals considering the whole sample of binaries: the first row is for the blue filter, and the second row is for the red filter. The third and fourth rows show the effect of applying a 3σ clipping to the data in order to compute the rms, for the blue and red filters, respectively. In these later plots, the dashed lines indicate the 3σ rms. In these figures we have added a color-coding to show the magnitude difference between the components, which adds a third dimension to the plots. Smaller, high-contrast circles depict smaller Δm, while larger, low-contrast circles depict the opposite. Blue circles were used for the blue filter plots, and red circles were used for the red filter plots. At the top of each panel, we include the mean residual value and its rms in the units of the corresponding ordinate.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: The same general descriptions for the third and fourth rows of Figure 7 are valid for this figure. Here, however, the first and second rows are for the range with ρ < 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4 (program stars), while the third and fourth rows are for the larger ρ binaries (mostly astrometric standards).
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Photometric precision: residuals (ordinate) vs. contrast (abscissa) and ρ for the 562 nm (left column) and 832 nm (right column) filters for all our binaries with observations in the two filters. The first row is for the whole sample, while the second row applies a 3σ clipping to compute the rms; in this case, the dotted lines indicate the 3σ rms. The third and fourth rows are similar, but as a function of mean ρ and magnitude difference. The color-coding in this figure is analogous to that of Figures 7 and 8. At the top of each figure, we include the mean residual value and its rms in the units of the corresponding ordinate.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Average ρ of the components (over all epochs) as a function of the mean Δm in the red filter for all the resolutions presented in Table 2. The left panel is for the whole sample, while the right panel is for objects with ρ less than 100 mas. In the left panel, the blue square indicates the only object with no detection in the red filter (STF 1998AB); for this we plot the blue filter contrast instead.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Example results for two astrometric calibrators: HIP 8998 (left panel, three epochs) and HIP 46454 (right panel, four epochs). In both cases blue and red measurements could be secured on each epoch (usually indistinguishable at the scale of the plots). The orbits shown are preliminary and are bound to be modified as more data are acquired. Indeed, these two orbits are currently listed as grade 2 in ORB6, with estimated periods of 167 and 118 yr, respectively.