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: Same as Figure 17, but for the whole sample.
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: Rotation diagrams for the whole sample, following the same style as in Figure 9.
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: Compact water spectral atlas for JDISCS targets (continued from Figure 28). Shown here are the disks that are consistent with a moderate to large cold water component in Figure 10.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: The correlation between the “order-of-magnitude mass-loss rate” estimated from the equivalent width of helium absorption and the energy-limited mass-loss rate. We first reported the correlation in M. Zhang et al. (2023a). This plot includes the same data as Figure 3 of M. Zhang et al. (2023a), except that we added the detections of TOI-1268b and TOI-2018b (J. Orell-Miquel et al. 2024), removed nondetections due to their proliferation, and added the results from this work. Note the extreme discrepancy between TOI-836b and c.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: “Residuals grid” for visit c2. The colors represent deviations, in percent, from the time-averaged mean flux at that wavelength (lower flux is yellower). The black triangles indicate the lines that we masked out before fitting a quadratic function to each row, which in turn was done to remove continuum variations.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: The molecfit telluric correction step. For visits c1 (upper left), c2 (upper right), and b (lower center), we plot an example uncorrected spectrum, the corrected version of that spectrum, and the transmission function used to make the correction. The wavelengths of the helium triplet are indicated in red.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Quadratic fits to the 0th and 80th rows of the “residuals grid” for visit c2. They are respectively examples of spectra with particularly low and particularly severe continuum variations.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Speckle ACF of the triple system HIP 57421 recorded on 2022.20 at 823 nm (in a negative rendering). The inner 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩18 pair is A,B, and the faint tertiary C is seen at a nearly orthogonal angle at 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩46. Green arrows show the direction of motion.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Preliminary visual orbits for HIP 76400 Aa1,Aa2 (left; P = 368.6 days, a = 19.5 mas) and HIP 101472 Aa,Ab (right; P = 354.9 days, a = 13.9 mas) derived by joint fitting of Zorro positions and available RVs. The insets show the Speckle power spectra recorded near maximum ρ at 832 nm, with the same orientation.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Power spectrum of HIP 58669 (left) and its model (right) taken on 2021.0359 at 832 nm. The fringes correspond to the A,B pair at a ρ of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩27. Note the loss of contrast and the inversion of fringe phase in the upper and lower areas, indicating the resolution of Aa,Ab.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Power spectrum of HIP 76400 taken on 2019.38 at 832 nm. The fine low-contrast fringes are produced by the companion Ab at 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩21, and the elongation indicates partial resolution of Aa1,Aa2 at 25 mas.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: The power spectrum of HIP 7869 (component A) recorded on 2020.90 at 832 nm (left), and its model accounting for the AD (right).
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Power spectrum of HIP 63377 taken in 2019.531 at 832 nm and showing resolution of the inner subsystem.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Procedure for estimating the velocity and quantity of blueshifted emission needed to reproduce different SC line profiles. In the top panel, the 0 km s−1 Gaussian component is illustrated by a solid gray line and the −30 km s−1 Gaussian components of varying amplitude by solid colored lines. The single Gaussian fits to their superpositions (not shown) are marked by the corresponding dashed colored lines. In the bottom panel, the degree of blueshifted emission is compared to its effect on the velocity of the fitted line. The nominal wavelength uncertainty of HST-COS is marked by the dashed gray line.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Schematic of fluorescent H2 (in blue) and [O I] λ6300 (in gold) emission in a CTTS. The magnitudes of median component wind velocities are represented by the lengths of the arrows. The arrows are placed according to the medians of the component emitting radii. We exclude the SCs of H2—[1,4] and the NCs of [O I] because their median velocities are near zero. We illustrate the [O I] emission layer above the H2 layer because it traces a hotter gas. The horizontal axis is in log scale. Adapted from M. Gangi et al. (2023).
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Distribution of component FWHMs with respect to RV-corrected component velocities. The [1,4] progression of fluorescent H2 is compared to [O I] λ6300 in the top panel, and the [0,2] progression is compared to [O I] in the bottom panel. Component velocities less than −25 km s−1 and FWHMs in excess of 180 km s−1 are cut off from the plot for easier visual comparison.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Correlations between component line broadening and the infrared index. We calculate the PCC for the SC distribution in each plot. We report the equation of the best-fit line (blue dot-dashed line) for statistically significant SC correlations. We do not plot the NC and BC distributions in the right panels because their emitting radii do not correlate strongly with the infrared index, and the scale of the y-axis is not favorable to visual inspection of small BC emitting radii.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Component velocity comparison of H2—[1,4] (left panels) and H2—[0,2] (right panels) with [O I] λ6300. SCs are in blue, NCs in orange, and BCs in green. Zero velocity is marked by a vertical dashed line. The top panels are copied from Figure 4, and the bottom panels are identical to facilitate comparison.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Correlation between H2 mass-loss rates and stellar mass accretion. Uncertainties on individual mass-loss estimates span at least an order of magnitude, which we represent with light-gray error bars on the right side of each panel. We include lines of constant mass-loss efficiency (0.01, 0.1, and 1) as dotted gray lines.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: One-to-one comparison of [1,4] and [O I] line kinematics for disks common to both samples, and with identical classification (i.e., SC or NC + BC). The gray dashed lines represent a hypothetical exact correspondence. We correct the H2 centroid velocities for stellar RV using the RVs reported in A. Banzatti et al. (2019).
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Correlations between H2 line kinematics and disk inclination for [1,4] and [0,2]. We mark the RV-corrected component velocity zero point with a light-gray dotted line (left panels).
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Upper panels: spatial distributions of the input (left panel) and recovered (right panel) fluxes of the [O III] λ5007 (blue), Hα (green), and [N II] λ6583 (red) emission lines in an arbitrary scale. Lower panel: example of the spectral modeling, showing the spectrum integrated across the field of view (FOV) of the simulated IFS data set (black solid line), together the best model for the stellar component (red solid line) and the set of strong ionized emission lines (blue solid line). The residuals of the subtraction of the stellar model (cyan solid line), and both models (yellow solid line) are also included. All the spectra are presented in the original flux intensities (middle panel), and normalized to one at 5000 Å (bottom panel). The orange vertical marks indicate the wavelengths at which the algorithm would attempt to extract the properties of a predefined set of emission lines using a weighted moment analysis, as described in the text. Shaded regions correspond to the overlapping regimes between the three arms of the spectrographs. The panel insets show zoom-in views in the wavelength range covered by a set of strong emission lines, including the [O II] doublet, Hδ, Hγ, Hβ, [O III], Hα, [N II], [S II], and the [S III] λλ9069, 9531 doublet.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Scheme of the LVM-DAP analysis flow for a single fiber spectrum, including the main procedures: (i) derivation of the nonlinear parameters of the stellar spectrum (v⋆, σ⋆, and AV,⋆); (ii) parametric derivation of the properties of the ionized gas emission lines (“EL”), including the flux intensity (fEL), velocity (vEL), and velocity dispersion (σEL); (iii) stellar-component synthesis, i.e., decomposition into a set of RSP templates; and finally (iv) nonparametric derivation of the properties of the emission lines, including the EW for each emission line (EWEL). RND and LM stand for the two methods included in pyFIT3D to fit the parametric models to the EL. RND corresponds to a pseudorandom sampling of the space of parameters and LM corresponds to the Levenberg–Marquardt, as explained in the text.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: PDF of the physical properties of stars (Teff, log(g), [Fe/H], and [α/Fe]) for the full template comprising 108 RSPs (black contours), together with the same distribution for three selected RSPs within the template (color contours) shown in Figure 3. Each panel shows the PDFs for a pair of physical properties: Teff–log(g) (top left); [Fe/H]–log(g) (top right); Teff–[α/Fe] (bottom left), and [α/Fe]–[Fe/H] (bottom right). In each panel each successive contour corresponds approximately to 1, 2, and 3σ.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Similar figure as the one shown in Figure 5, adopting the same nomenclature, symbols, and color schemes, for the realistic simulation performed using one LVM pointing on the Rosetta Nebula. White hexagons inside the IFU correspond to broken and low-transmission fibers in the input data.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the value of the physical properties (Teff, log(g), [Fe/H], and [α/Fe]) of one arbitrarily selected star of within the MaStar catalog as derived by CoSHa (blue star) and the PDF recovered by the DAP (red contours). The PDFs for the full template comprising 108 RSPs, already shown in Figure 4, have been included for reference (black contours). Each panel shows the PDFs for a pair of physical properties: Teff–log(g) (top left); [Fe/H]–log(g) (top right); Teff–[α/Fe] (bottom left); and [α/Fe]–[Fe/H] (bottom right). In each panel each successive contour corresponds approximately to 1, 2, and 3σ.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Subset of the spectra included in the template comprising 108 RSPs created by clustering in the observational space the 1235 RSPs whose properties are shown in Figure 2. Each black line shows the final RSP spectrum, created by averaging all the spectra belonging to the same cluster, represented by the orange lines. Spectra are ordered by blue to red, from the bluest (bottom left) to the reddest (top right), arbitrarily scaled to avoid overlapping. The ID number of each RSP within the considered template is included at the right end of each spectrum.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the simulated and recovered parameters for the emission lines based on the nonparametric analysis described in Section 3.1, for the ad hoc realistic simulations described in Section 4.2. A total of 326,400 emission lines were included in the simulation. We represent here the results for the 44,979 ones with an S/N > 3. Each panel shows the distribution the flux intensity (top left), EW (top right), velocity (bottom left), and velocity dispersion (bottom right). In each panel, black solid circles represent the individual values and contours represent the density, encircling 95%, 65%, and 15% of the points, respectively. Dark red dashed–dotted lines represent the one-to-one relation.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the stellar physical parameters (Teff: top left; log(g): top right; [Fe/H]: bottom left; and [α/Fe]: bottom right) estimated by the LVM-DAP using an RSP library with just 108 templates, and the values reported by CoSHa for the ∼19,000 individual MaStar stars with S/N > 10. Contours, symbols, and lines in each panel have the same meaning as those in Figure 7.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Distribution of the physical properties derived using CoSHa for 22,773 stars extracted from the MaStar stellar library (gray solid line and density contours), together with the average properties for the 1235 RSPs created by clustering those MaStar stars in the space of physical properties using a regular grid (colored stars). Left (right) panel shows the distribution in the log(g)–Teff ([α/Fe]–[Fe/H]) plane, with colors tracing [Fe/H] (Teff). In each panel successive contours encircle 95%, 65%, and 25% of the MaStar stars, respectively.
Paper: Extinction Distributions in Nearby Star-resolved Galaxies. I. M31
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Stellar number density distributions in individual color–color diagrams for dwarfs (blue contours) and giants/supergiants (red contours) from the APOGEE catalog, along with theoretical distributions generated using the CMD 3.7 web interface (green contours). The blue, black and green lines represent fifth-order, third-order, and fifth-order polynomial fits, respectively, to the median values obtained after 3σ clipping.
Paper: Extinction Distributions in Nearby Star-resolved Galaxies. I. M31
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Example of a multisolution situation. The orange point represents the observed colors of a tracer in color–color space. The red line is parallel to the reddening vector and intersects the stellar locus at two points (Solution 1 and Solution 2). Solution 1 corresponds to a star at a shorter distance with greater extinction, while Solution 2 represents a more distant star with smaller extinction.
Paper: Identification of Possible Stellar Companions via Speckle Interferometry in a Sample of Be Stars II
Authors: C. A. Guerrero, T. B. Souza, M. Borges Fernandes, A. D. Guajardo Jurado
Figure caption: Autocorrelation function of the previously known double systems. At the top, we show the average of our calculated angular separation, while at the bottom, we show the Julian epoch in which these objects were observed.
Paper: Extinction Distributions in Nearby Star-resolved Galaxies. I. M31
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Foreground extinction distribution toward M31 with a resolution of approximately 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩7.
Paper: Identification of Possible Stellar Companions via Speckle Interferometry in a Sample of Be Stars II
Authors: C. A. Guerrero, T. B. Souza, M. Borges Fernandes, A. D. Guajardo Jurado
Figure caption: The solid line is the revised orbit of HD 41600 (WDS 06073 + 2641). Axis units are in arcseconds and the dashed line represents the previous orbital solution by R. Mante (2002).
Paper: Identification of Possible Stellar Companions via Speckle Interferometry in a Sample of Be Stars II
Authors: C. A. Guerrero, T. B. Souza, M. Borges Fernandes, A. D. Guajardo Jurado
Figure caption: Autocorrelation function of new interferometric pairs identified in Be stars.