adsabs/AstroCLIMB huggingface dataset:
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: We show the mass estimates derived from our 5σ contrast limits (in M Jup) in each gap/cavity (specified in astronomical units above each system designation) as the bars colored by radial distance from the host star. The bars therefore represent the range of masses that we would have been sensitive to given our observations. The ages for HL Tau, ISO-Oph 2, and SR 21 are lower than the youngest age in the AMES-Cond grid (1 Myr), therefore we show the masses assuming an age of 1 Myr as an upper limit to the ages, as a younger system would correspond to smaller mass. We also show the associated masses assuming the AMES-Dusty models when the masses were within the grid in purple. There is a subset of systems that have estimates of planetary masses not ascertained via the Lodato et al. (2019), Wang et al. (2021), and Zhang et al. (2018) methods. The putative companion in CQ Tau is detailed in Wölfer et al. (2021), the putative companion in GM Aur is detailed in Huang et al. (2020), and the putative companion in HD 141569 is detailed in Konishi et al. (2016). The putative companion in each of the two gaps in HD 169142 have mass estimates of between 0.1 and 1 M Jup for the inner planet and 1–10M Jup for the outer planet, so we show the lower limits for these masses (Fedele et al. 2017). The putative companion in SR 21 is detailed in Muro-Arena et al. (2020). The putative companions in TW Hya  and LkCa 15 are detailed in Dong & Fung (2017). Additional details on NIRC2 observations of TW Hya with the vortex coronagraph can be found in Ruane et al. (2017). We show the expected planet masses as points. For the locations of the central cavities, we generally use the inner edges of the dust rings.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: We show a comparison of the mass estimates from the ALMA data and our observational mass limits for the subset of our systems observed as part of the DSHARP survey (Andrews et al. 2018) or the survey of the Taurus molecular cloud (Long et al. 2018). We show the ALMA-derived planet masses (in M Jup) as the points and the mass estimates derived using the AMES-Cond models from our 5σ contrast limits as the orange bars for each observed gap from the ALMA data (specified in astronomical units as the numbers above each system designation). The bars therefore represent the range of masses that we would have been sensitive to given our observations. The ages of Elias 2–20 and Elias 2–24 are lower than the youngest age in the AMES-Cond grid (1 Myr). Therefore, we show the masses assuming 1 Myr as upper limits to the ages, as younger systems would result in smaller masses. We also show the associated masses assuming the AMES-Dusty models when the masses were within the grid in purple.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison of the contrasts achieved using the pyKLIP and VIP reductions. The solid lines are the median contrasts of all of the contrast curves and the shaded regions represent the range of contrasts. We use ADI for the pyKLIP reductions and a combination of ADI and RDI for the VIP reductions. The improved performance of the VIP reductions as compared to the pyKLIP reductions is likely due to the additional observation-specific optimizations that were done using VIP. However, the contrasts are still comparable, showing the robustness of our calculated contrasts.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Optimal contrast curves for our sample of protoplanetary disks colored by the ﹩L^{\prime} ﹩ magnitude. Each line is the most optimal 5σ contrast for a different disk. The contrast curves at select separations are shown in Table B1 in the Appendix.(The data used to create this figure are available.)
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Companion mass upper limits (computed using the AMES-Cond model grid) as a function of the separation for the systems studied herein which did not have clear locations where a planet would be present or the locations of a gap or cavity were outside of our separation range. When the age of the system is lower than the youngest age in the AMES-Cond grid, we assume an upper limit of 1 Myr.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Disks in our survey showing evidence of structure, which is indicative of scattered light disks. We show the 1σ , 2σ , and 3σ ALMA contours (from references in Table A1) overlaid on our 3.8 μm images for reference. North is up and east is left in all of the images. We show the reduction method that optimizes the appearance of the extended structure.
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: A map of the average sensitivity of our survey in planet mass (calculated using the AMES-Cond and AMES-Dusty models) vs. separation in astronomical units calculated using Exo-DMC (Bonavita 2020).
Paper: A Survey of Protoplanetary Disks Using the Keck/NIRC2 Vortex Coronagraph
Authors: Nicole L. Wallack, Jean-Baptiste Ruffio, Garreth Ruane, Bin B. Ren, 彬 任, Jerry W. Xuan, Marion Villenave, Dimitri Mawet, Karl Stapelfeldt, Jason J. Wang, Michael C. Liu, Olivier Absil, Carlos Alvarez, Jaehan Bae, Charlotte Bond, Michael Bottom, Benjamin Calvin, Élodie Choquet, Valentin Christiaens, Therese Cook, Bruno Femenía Castellá, Carlos Gomez Gonzalez, Greta Guidi, Elsa Huby, Joel Kastner, Heather A. Knutson, Tiffany Meshkat, Henry Ngo, Sam Ragland, Maddalena Reggiani, Luca Ricci, Eugene Serabyn, Taichi Uyama, Jonathan P. Williams, Peter Wizinowich, Zoe Zawol, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison of the planet-to-star flux ratio of the point sources in Figure C1 determined from the VIP reductions vs. the planet-to-star flux ratio in the same location in the pyKLIP reductions. A perfectly consistent flux ratio is designated by the dotted line.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Autocorrelation as a function of frequency lag for LS, its filtered version using a moving-mean boxcar of width K, and mtNUFFT with NW = 4 and K = 7 parameters. We see that the mtNUFFT autocorrelation is similar to that of the moving-mean boxcar version of LS. Both of these power spectrum estimates are correlated within the 2W frequency range (marked by the orange dotted line), whereas the LS estimates not. All the periodograms have ≈0 correlations beyond this 2W range.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Flat fields of the blue (left) and red (right) spectrograph detectors in standard resolution mode, showing the orders from top to bottom. The orders are not numbered for clarity. The zoom-in to the bottom left shows the individual fibers, resolved in order 72 and numbered. A cut across the order is also shown, displaying the profiles of the individual fibers and revealing the image quality of the final spectrum. The fiber numbers within each order have the same convention and can be traced to the pseudo-slit image (Figure 4) and to the initial entrance for light in the IFU as seen in Figure 3. Also visible is the extremely low interorder background and scattered light in the final echellogram.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Simplified block diagram, depicting the data flow architecture during GHOST observations at Gemini South. The top panel shows how the various software systems coordinate to send commands to the top-level computer. The TLC then controls the various instrument subsystems to produce a multi-extension FITS file. The bottom panel shows the structure of the MEF file outputted.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Spiral search acquisition sequence dialog. When flux levels are below a predetermined detection threshold on the presumed target coordinates, then an automated sequence of offsets is initiated around the initial location. The concentric circles indicate positional errors of 1σ, 2σ, and 3σ from the center respectively, where σ is 1″. In this example, the search has been initiated. The highest flux level was found at position 4 in the previous iteration as shown in the dialog at the top. In the current iteration, positions 0–3 have been completed (in orange), and 4 is next to be taken (in red) in the process. The IFU will now repeat until the center of the IFU has the highest flux level.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: A comparison of the performance of the Gemini integration time calculator in measuring SNR per resolution element. (a) Comparison of the observed spectra (blue and red) taken in standard resolution, target and sky modes with a binning of two in the spectral direction. The ITC simulated spectrum in approximately similar seeing, cloud cover, and sky brightness conditions at the same instrument settings in also shown (gray solid line). (b) The same comparison, but for the high-resolution mode unbinned. Observations are not corrected for telluric contamination.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Measured resolution in the HR mode displayed in the echelle format for the blue (top) and red (bottom) detectors. The ordinate refers to the order number, and abscissa the pixel value. Standard-resolution mode follows roughly similar resolution patterns on the detector. Measured line locations are marked. Corners of the map are extrapolated and not necessarily representative of the achieved resolution. The color bar refers to the achieved resolution, smoothed and mapped using a multi-quadratic function.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Relative radial velocity shift measured over a duration of six nights on the standard star HD 21693 in both standard (solid black squares) and high-resolution mode (light gray circles). The dashed and dotted lines indicate variations of 50 and 100 m s−1, respectively.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Measured total throughput of GHOST at Gemini South from selected spectrophotometric observations, from top of the atmosphere to the detector. For completeness, note that the values on the vertical axis are percentages. The instrument during these observations was located at the bottom port. When mounted on the side port, the throughput is slightly lower owing to the addition of the science fold mirror reflection. The drop around 530 nm at the dichroic is also visible.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Mean pixel drift compared to the grating temperature and enclosure pressure over two nights in 2024 April. Dotted lines mark the change in pixel value in the blue detector (blue) and red detector (red). The grating temperature (green) is given in units of kelvin, and the enclosure pressure (black) in hPa. All values are normalized to the initial value, with pressure divided by a factor of 20 for display.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: The aperture transmission factor as a function of seeing, accounting also for filling factor losses in the IFU configuration. Shown also are the seeing bins adopted at Gemini South during queue mode.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Mean and standard deviation of outer vs. inner stability borders in units of log10 of the binary semimajor axis. The color scale refers to the binary orbit eccentricity (top left), the planet’s orbital eccentricity (top right), the binary mass ratio (bottom left), and the mutual inclination (bottom right). Stability limits depend strongly on the planetary orbital eccentricity, which accounts for most of the variance in the system. Stability borders also show roughly the same sensitivity to the orbital eccentricity of the binary star, the binary mass ratio, and the inclination of the system.