adsabs/AstroCLIMB huggingface dataset:
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Redshifts estimated with LEPHARE. Black solid line: sample of GC candidates before DESI and GAIA rejections. Blue solid line: sample after DESI and GAIA rejections. Red solid line: sample of bona fide GC candidates. Black dashed line: the redshift of NGC 1399, the dominant galaxy of Fornax. Blue and red dashed lines: lower and upper range taking into account the mean errors for the redshift estimations.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: g − i)0 color distribution for the BF-GCC sample. The black solid line is the unimodal fit returned by the GMM analysis and blue and red solid lines are the bimodal fit returned by the GMM analysis. The green dashed line is the sum of the red and blue fits.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Observational properties in the 106 FOVs in the i band. In the first row of panels, we show the parameters: AIRMASS, SATUR_LEVEL, MEDIAN, and RMS vs. the total number of sources detected in each FOV. In the second row of panels, we show all of the FOVs in (RA,DEC) space with a color coded for each parameter: AIRMASS, SATUR_LEVEL, MEDIAN RMS. The third row of panels shows the FWHM and ratio of the GCC divided by the total sources detected in each field.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Spatial distribution in RA,DEC (J2000) coordinates for the BF-GCC sample (red dots). Galaxies from the literature are indicated with blue circles and green empty squares. The black empty circles are the multiples (0.5, 1, 2, 3) of the Rvir centered in NGC 1399. The black solid point represents the center of NGC 1399 galaxy. In the bottom panels, we show the GCs distribution smoothed with a Gaussian kernel (blue distribution) of the BF-GCC on the left, and including only objects identified as “PSF” by DESI on the right; see the text for more details.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Colors and GCLF at different Rvir  0.5, 1, 2, and 3 (from the top to bottom panels). The first and second columns are the (g − i)0 and (g − z)0 colors; the color code is the same as in Figure 11. The third column shows the i-GCLF; the color code is the same as in Figure 13.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Sample of galaxies (green ellipses), GC candidates (red circles), and spec-GCs recovered in the S-PLUS i band (yellow circles). All images are snapshots in the i band from S-PLUS and are aligned such that north is up and east to the left, and the angular size equivalent to 100″ (green arrows) is shown.
Paper: The S-PLUS Fornax Project (S+FP): Mapping Globular Clusters Systems within 5 Virial Radii around NGC 1399
Authors: Luis Lomelí-Núñez, A. Cortesi, A. V. Smith Castelli, M. L. Buzzo, Y. D. Mayya, Vasiliki Fragkou, J. A. Alzate-Trujillo, R. F. Haack, J. P. Calderón, A. R. Lopes, Michael Hilker, M. Grossi, Karín Menéndez-Delmestre, Thiago S. Gonçalves, Ana L. Chies-Santos, L. A. Gutiérrez-Soto, Ciria Lima-Dias, S. V. Werner, Pedro K. Humire, R. C. Thom de Souza, A. Alvarez-Candal, Swayamtrupta Panda, Avinash Chaturvedi, E. Telles, C. Mendes de Oliveira, A. Kanaan, T. Ribeiro, W. Schoenell
Figure caption: Same color code as in Figure 13.
Paper: Size Constraint on Hayabusa2 Extended Mission Rendezvous Target 1998 KY26 via VLT/VISIR Nondetection
Authors: Jin Beniyama, Thomas G. Müller, Marco Delbo, Eric Pantin, Olivier R. Hainaut, Marco Micheli, Michaël Marsset
Figure caption: Final stacked image with synthetic point source objects with flux densities of 5 mJy, 3 mJy, 2 mJy, and 1.5 mJy inserted. The flux density of the synthetic sources are indicated in the accompanying text.
Paper: Size Constraint on Hayabusa2 Extended Mission Rendezvous Target 1998 KY26 via VLT/VISIR Nondetection
Authors: Jin Beniyama, Thomas G. Müller, Marco Delbo, Eric Pantin, Olivier R. Hainaut, Marco Micheli, Michaël Marsset
Figure caption: Flux predictions (in mJy) for 1998 KY26 for 2024 May 27 based on different model assumptions and for a wide range of object sizes. The VISIR/B10.7 band point-source detection limit is indicated as a horizontal dashed line. The various model parameters are explained in the text.
Paper: Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: The values of χ2 × MAD as a function of mean r-band magnitudes for the SDSS DR16 stars with more than 10 data points on the LOT r-band light curves. A variable star candidate clearly stands out against the constant stars with χ2 × MAD ∼ 0.05. Three bright stars with ﹩\bar{r}\sim 19.6﹩ mag and χ2 × MAD ∼ 0.25 appear to be low-amplitude variable stars. However, based on their light curves and locations on the CMD, they are clearly not RR Lyrae, nor the interest of this work.
Paper: Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: A coadded image by median-combined all of the LOT images using SWARP (E. Bertin et al. 2002). Location of the candidate variable star is also marked on the image. The cyan contours represent {1, 2,​​​​​​ 3, 4} × rh (with parameters taken from W. Cerny et al. 2025).
Paper: Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Left panel: folded light curves for the candidate variable star assuming it is an ab-type RR Lyrae. The dotted curves are the poorly fit template light curves by setting the amplitudes as a free parameter (in addition to the mean magnitude). In contrast, the solid curves are the best-fit template light curves by setting the amplitude either as a free parameter (in the r band) or as a fixed parameter (in the gr band; see text for more details). Right panel: comparison of the extinction-corrected colors and the reddening-free Q-index for the candidate variable star to the ab-type RR Lyrae in the globular clusters (cyan points; adopted from C.-C. Ngeow et al. 2022). The foreground extinction for this candidate variable star was obtained from using the Bayerstar2019 3D reddening map (G. M. Green et al. 2019), together with the dustmaps (G. M. Green 2018) code, which returned an extinction value of 0.054 ± 0.004 mag.
Paper: Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: The gri-band phased light curves for the potential RR Lyrae identified in Section 2.2. The cyan filled circles and red triangles are the data points retrieved from ZTFDR22 and PS1DR2, respectively. The black curves are the best-fit template light curves derived in V. F. Braga et al. (2024).
Paper: Candidate RR Lyrae Associated with the Ultrafaint Dwarf Galaxy Aquarius III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Two examples of the synthetic CMD without (left panels) and with (right panels; shown as red squares) RR Lyrae. These synthetic CMD were constructed using the BaSTI web tool, which also provide the identification of RR Lyrae from the synthetic stars. These four synthetic CMD have a slightly different input SFR scales and resulted a different MV (see text for more details).
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Flow diagram of our planet detection algorithm. We used the same algorithm for detecting planets (Section 4) and for computing the completeness (Section 6). We began by initializing an orbital model with the RV data and the ephemerides of any known transiting planets. We then determined whether the data supported the inclusion of a trend—that is, if a trend model was favored over a flat model by ΔBIC > 5—after which we added a new planet to the model. We computed (ΔBIC) between the starting model and a model with a trial planet over a dense grid of trial periods. If the maximum ΔBIC exceeded 30, we performed a final model comparison test to select a model with a planet, a trend, or both. We iteratively added planets to the model in this way until no more were found. For the injection/recovery experiments described in Section 6, we began with the final model from Section 4, to retain any planets found during the initial search. We then injected a synthetic planetary signal into the data and began the recovery at the trend test step (outlined in red). When the search terminated, we checked whether the injected signal was recovered, either as a planet or as a trend, and recorded the result.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Stellar and transiting planet parameters of the Distant Giants Survey. (a) Metallicity and V-band magnitude of stars with companions detected as resolved orbits (blue squares), stars with companions detected as accelerations (red diamonds), and stars with no detected companions (black circles). The unfilled circles show other systems in the larger TKS. The other panels are same as (a) but for (b) ﹩V\sin i﹩ and ﹩\mathrm{log}{R}_{{\rm{H}}{\rm{K}}}^{{\prime} }﹩, (c) stellar radius and temperature, and (d) transiting planet radius and orbital period. For multitransiting systems, we show the first planet to pass our survey filter (lowest TOI number).
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: CSs and their DG companions. Masses and periods of exoplanets from our survey (bold squares) and the NEA (faded circles) are shown for context. The red/blue points indicate planets discovered using the transit/RV method. The red squares show the true masses of transiting planets in the Distant Giants Survey measured by RVs (A. S. Polanski et al. 2024), while the blue squares show minimum mass measurements (﹩M\sin i﹩). For systems with multiple transiting planets, we show the parameters of the transiting planet with the lowest TOI designation that passed our filters. The red squares with yellow borders indicate systems in which we detected a linear/quadratic trend. The giant planets in our sample are connected to the inner planet in their system by a black line. The box corresponds to our nominal definition of a DG.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Masses and orbital spacings of the planets in each system in our survey. The systems are ordered according to the semimajor axis of the innermost transiting planet. Transiting planets are shown with black markers, and nontransiting planets are colored according to their eccentricity. The marker sizes are proportional to the square root of the planet true mass (for transiting planets) or minimum mass (for nontransiting planets). We use red borders to indicate the planets that meet our definition of a DG. For systems with RV trends, we place a red triangle at a separation corresponding to 6 yr, the approximate maximum period for which we could resolve a Keplerian orbit. Based on Figure 4 of L. M. Weiss et al. (2024).
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: RV observations of the Distant Giants Survey. In total, we collected 1990 RVs from Keck/HIRES (red squares) and 2036 observations from APF/Levy (gray circles) between 2020 August 1 and 2024 January 31. Note that a few targets had prior RVs that are not shown. TOI identifiers are shown in the left margin, ordered by R.A. Each year label on the x-axis marks February 1, the first day of the “A” observing semester. The typical target in our survey is not accessible from Keck for about three months per year, resulting in the diagonal cadence gaps. The eruption of Mauna Loa in 2022 November, as well as unrelated damage to the lower shutter of the Keck I dome between 2022 November and 2023 May, resulted in a substantial decrease in observation cadence for targets between R.A. ∼ 16 and 22 hr, which did not reach elevations >40∘ during this period.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: An illustration of our decentralized framework in the context of two partitions ﹩{\,{\rm{V}}}_{{ \mathcal L }}﹩ and ﹩{\,{\rm{V}}}_{{ \mathcal H }}﹩. We reconstruct two full-resolution images in parallel, achieved by sharing the filtered deconvolved residuals, ﹩{{\rm{\Phi }}}_{{ \mathcal H }}^{n}﹩ and ﹩{{\rm{\Phi }}}_{{ \mathcal L }}^{n}﹩, between different nodes after each major cycle, denoted as MC in the figure. The deconvolved residuals are filtered both for normalization purposes, as well as to ensure that only spatial frequencies from their corresponding domains are present. Low- and high-resolution deconvolved images are produced after the first major cycle, denoted as ﹩{\bar{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal L }}}^{\,1}﹩ and ﹩{\bar{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal H }}}^{\,1}﹩ respectively. Afterwards, full-resolution deconvolutions ﹩{\bar{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal L }}}^{n}﹩ and ﹩{\bar{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal H }}}^{n}﹩, where n > 1, are produced. The final reconstructed images of their respective nodes, ﹩{\hat{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal L }}}﹩ and ﹩{\hat{\iota }}_{{\,{\rm{V}}\,}_{{ \mathcal H }}}﹩, are then combined to produce the final reconstructed image ﹩\hat{\iota }﹩.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: A high-level overview of the radio-interferometric pipeline. A reconstructed image ﹩{\hat{\iota }}^{n}﹩ is compared to the measured visibilities v in the de/gridding step, which outputs the residual ﹩{\tilde{\iota }}^{n}﹩ in the spatial domain. This is passed to the estimation algorithm, which generates ﹩{\bar{\iota }}^{n}﹩, an estimate of ﹩{\tilde{\iota }}^{n}﹩ without the effects of the measurement operator F†GG†F. The current reconstructed image ﹩{\hat{\iota }}^{n}﹩ is then updated to ﹩{\hat{\iota }}^{\,n+1}﹩ by adding ﹩{\bar{\iota }}^{n}﹩ to it. Since the estimation algorithm is usually iterative, the overall pipeline often has a major–minor loop structure.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: Time vs. accuracy for all four of our data sets, with each circle representing a major cycle. The left two simulated data sets use S/N in dB for accuracy, whereas the right two real data sets use the L2 norm of the per-pixel Wasserstein distances between the noisy reference image and the current residual, computed within a 5 × 5 sliding window because we only have one realization of the residual.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: The full set of visibilities is partitioned according to domains ﹩{ \mathcal L }﹩ (orange), which contains the low spatial frequency visibilities, and ﹩{ \mathcal H }﹩ (green), which contains the high spatial frequency visibilities. These are not mutually exclusive but rather have an overlap region, which is denoted in cyan, and is defined using ℓ, which is the radius of a circle bisecting ﹩{ \mathcal L }\cap { \mathcal H }﹩, and δ, the half-width of ﹩{ \mathcal L }\cap { \mathcal H }﹩.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: The breakdown of computation time taken by the various subprocesses for our four methods.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: Dirty images of the four data sets we use for our experiments. The top two are simulated, whereas the bottom two are real observations performed with ALMA and the Very Large Array, respectively.
Paper: A Decentralized Framework for Radio-interferometric Image Reconstruction
Authors: S. Wang, S. Mignot, S. Prunet, L. Di Mascolo, M. Spinelli, A. Ferrari
Figure caption: A percentage breakdown of processing time used by the various subprocesses of the L1 method across our four data sets.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Top: we compare the 1σ confidence intervals from a retrieved model spectrum dominated by water absorption and excluding methane (red) to an alternate scenario where the atmosphere has no water and is dominated by methane absorption (blue). The points with error bars are the observed transmission spectrum, as in Figure 3. We performed a leave-one-out cross-validation analysis (LOO-CV) on the observed spectrum to evaluate each point’s relative evidence for the fiducial model. The resulting Δelpdi values are presented as the coloring of each data point. For reference, the bluest point has Δelpdi = −1.1 and the reddest point has a Δelpdi = 1.7. Bottom: we compare the data-model residuals relative to the water-dominated/methane-free model, shown by the black points, to the difference between the methane-free and water-free models, shown as the gray shaded region.