adsabs/AstroCLIMB huggingface dataset:
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Predicted delay time, Δt, for light echoes from AB Aur b. Inclinations from 0°–90° are shown in steps of 10°. Left panel: the protoplanetary disk inclination (23° ± 2°), orientation of the disk’s rotation axis (–36° ± 5°), and position of AB Aur b in its orbit correspond to a constraint in the expected delay time. These are represented here with 1σ, 2σ, and 3σ contours in joint constraints of Δt as a function of ΔPA, the absolute difference between the companion PA and the longitude of ascending node. Right panel: marginalized distribution delay times for AB Aur b. Our best estimate is Δt = 8.8 ± 0.6 hr.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Time delay of light echoes as a function of orbital phase (ω + ν(t)). Time delays are shown in units of r/c, which is the time it takes for light to travel from the star to the companion. Inclinations from 0°–90° are shown in steps of 10°. Depending on the inclination and location in the orbit, the time delay can reach a minimum of 0 and a maximum of 2r/c, depending on the three-dimensional geometry of the system. For the application to accreting protoplanets, this highlights the need to determine the disk inclination, the disk orientation, and the current position of the companion in its orbit to accurately compute the expected time delay for a light echo.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Normalized TESS light curves of AB Aur from Sectors 19, 43, 44, 59, 71, and 86. The variability within each Sector of a few percent suggests only modest changes in accretion rate over month-long baselines.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Light curves of AB Aur in F656N across the five epochs of this experiment. Light-curve timescales are with respect to the midpoint of Orbit 1, and photometry has been normalized to the average flux in Orbit 1. Overall, AB Aur is quite stable, with low-amplitude changes in Hα at the few-percent level evident across the 15–17 hr baseline of each epoch.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: X- and Y-positions of the 23 AORs observing KF09T1 with the 4.5 μm channel of Spitzer, showing that only a small fraction of the data overlapped with the fixed-sensitivity map. The “Sweet Spot” marked on the plot is from J. G. Ingalls et al. (2012).
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Comparison of the data best-fit results at 3.6 and 4.5 μm to modeled phase curves for WASP-121b. The top row compares to RM-GCM results with and without clouds and magnetic effects. The bottom row compares to Bell_EBM fits.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Temperature maps at the 0.1 bar pressure level for each of the WASP-121b GCMs, with wind patterns overlaid. For the two cloudy models, contours of integrated 4 μm cloud optical depth above 0.1 bar are displayed in the bottom row. In magnetic models, the eastward equatorial jet is significantly disrupted, reducing the hotspot offset and decreasing the efficiency of heat transport to the nightside, increasing day–night contrast. In cloudy models, clouds are entirely absent from the dayside but present on much of the nightside above 0.1 bar.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Comparison of our best fit to the data with model results, similarly to Figure 9, for WASP-77Ab. Phase amplitudes and dayside thermal fluxes from RM-GCM results are excessive compared to the data. The simplified Bell_EBM is able to reproduce measured fluxes by assuming an atypically high Bond albedo.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Best-fit phase curves for WASP-121b at 3.6 μm (top) and 4.5 μm (bottom), with resulting residuals. The black curves show the best-fit phase, eclipse, and transit models. The gray curves are a sampling of 100 MCMC solutions for the phase-curve parameters to visualize the solution error. The dotted vertical line shows the center of first eclipse, and the vertical blue bar indicates the calculated phase offset with error.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Best-fit phase curves for WASP-77Ab at 3.6 μm (top) and 4.5 μm (bottom), with resulting residuals. The black curves show the best-fit phase, eclipse, and transit models. The gray curves are a sampling of 100 MCMC solutions for the phase-curve parameters to visualize the solution error. The dotted vertical line shows the center of first eclipse, and the vertical blue bar indicates the calculated phase offset with error.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: x- and y-centroids (top) and corresponding raw (uncorrected) flux (bottom) for all phase curves analyzed in this study. In the top panel the AOR gaps are marked by vertical lines, and in the bottom panel phases of ±0.5 (secondary eclipse) and 1.0 (transit) are marked to guide the eye.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: BLISS maps for the data sets analyzed in this work. The color bar denotes the relative sensitivity of a given subpixel element. The 4.5 μm observations also show the extent of our fixed-sensitivity map in the brown shaded region. The 3.6 μm map for WASP-77Ab (lower left) shows the pre-clipped data. The data removed for analysis are depicted in gray. Dashed lines denote the edges of a pixel (where relevant), with axis labels in subpixel units.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Mean zonal wind speeds (eastward = positive) in each of the GCM models used in this work as a function of latitude and pressure. Different columns represent our different model cases, and the rows correspond to WASP-77Ab and WASP-121b, respectively. Models without magnetic drag develop strong equatorial jets. Including magnetic drag disrupts these jets on the dayside, where the ionization fraction is significant, reducing the strength of the mean zonal wind. For each case we see generally low vertical velocity gradients at 0.1 bar, close to where both Spitzer channels probe.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Comparison of constant (navy blue) vs. sinusoidally varying (cyan) fits to the 4.5 μm observations of KF09T1 which overlapped with the 4.5 μm fixed-sensitivity map. Evident in the plots is the need for some amount of variability to model the stellar flux.
Paper: An Analysis of Spitzer Phase Curves for WASP-121b and WASP-77Ab
Authors: Brian Davenport, Thomas Kennedy, E. M. May, Emily Rauscher, Eliza M.-R. Kempton, Isaac Malsky, Kevin B. Stevenson, Jacob L. Bean, Megan Weiner Mansfield
Figure caption: Plot of period vs. phase offset for 3.6 μm (top) and 4.5 μm (bottom) Spitzer data. The purple lines show calculated best-fit trends (with error), and the cyan lines show constant-value (no trend) fits. The solid-lined, darker shading highlights the fit preferred by BIC. The stars represent WASP-121b and WASP-77Ab. Each planet is colored by equilibrium temperature.
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: First panel to the left: i-band magnitude distribution of the GC spectroscopic sample from the literature (blue histogram) and GCs recovered with S-PLUS (black histogram). From left to right, we show Fornax GCs PSF magnitude comparison in the g band (second panel), r band (third panel), and i band (fourth panel). In the last three panels, we show the S-PLUS GC magnitudes vs. the spectroscopic GC magnitudes (A. Chaturvedi et al. 2022). The black solid line in the top panels is the identity line, while the black dashed lines in the bottom panels mark where the differences between magnitudes (Δmag = SPLUS − Ch22) are equal to zero.
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: Structural parameters used for the selection vs. i-band magnitude. All detected sources are shown as small black dots, and spec-GC are depicted in yellow. In all panels, the horizontal magenta dashed lines define the selection region of GC candidates.
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: Data coverage of the 106 S-PLUS pointings in Fornax. Cloud of black dots: all detections in each FOV. A total of 3,085,787 sources was detected. A darker color implies a greater number of detected sources. Black solid lines: limits of each pointing. Blue legends: in the center of each pointing, we show their key names from S-PLUS. Red symbols: indicate the central coordinates of some of the brightest galaxies in Fornax. Magenta and cyan squares: represent the FOVs of FDS (E. Iodice et al. 2016) and EUCLID (T. Saifollahi et al. 2024) studies. The image is aligned such that north is up and east is to the left.
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: Example of the subtraction of the light profile of the galaxies. Left panel: S-PLUS g-band image of NGC 1399. Center panel: galaxy model. Right panel: residual image. All images are aligned such that north is up and east is to the left.
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: Left panel: color–color diagram (r − i)0 vs. (g − i)0 of all cluster candidates (SCs, black dots). Sources having (g − i)0 ≥ 0.65 mag and −0.10 mag ≤ (r − i)0 ≤ 0.70 mag are considered GC candidates (GCC, red dots). The chosen color cut separates clusters older than 3 Gyr from the younger ones for unreddened SSPs. Right panel: color–color diagram (u − i)0 vs. (g − i)0 showing the u-selected cluster candidates (SCs). Objects displaying (g − i)0 ≥ 0.65 mag are GC candidates (BF-GCC, red dots), and bluer objects are possible young star cluster candidates (rYSC, black dots). The bluest color that a classical GC can have (corresponding to Z = 0.0004 and to an age of 12 Gyr) is marked by a rose solid triangle ((g − i)0 ∼ 0.6 and (u − i)0 ∼ 1.9). The reddened young star clusters that displays colors typical of GCs are contaminants and are identified by open cyan circles. In both panels: the reddening vector with AV = 1 mag is represented by the black arrow. The evolutionary loci of SSPs from G. Bruzual & S. Charlot (2003) for different metallicities using a Kroupa IMF are shown by solid curves of different colors, following the color notation shown in each panel. The spectral GCs (spec-GC) are depicted by yellow circles.
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: Top panel: color histogram of cluster candidates. The black line shows the color distribution over the entire range of magnitudes, whereas the green histogram shows the distribution for bright (﹩{M}_{{i}_{0}}\,\leqslant \,﹩−11.5 mag) clusters. The blue dashed vertical line at (g − i)0 = 0.65 mag separates foreground stars, background galaxies, and young cluster candidates from GCs. Bottom panel: ﹩{M}_{{i}_{0}}﹩ vs. (g − i)0 CMD of all cluster candidates in the 106 Fornax pointings. Sources having (g − i)0  ≥  0.65 mag are GC candidates (red small open circles), bluer objects are foreground stars, background galaxies, and young cluster candidates (black points), and all of the detections are represented by a cloud of gray dots. The evolutionary locus of the single stellar population (SSP) models from G. Bruzual & S. Charlot (2003) for a single metallicity Z = 0.001, two values of masses of 1 × 106 ﹩{{ \mathcal M }}_{\odot }﹩ (blue solid line) and 5 × 106 ﹩{{ \mathcal M }}_{\odot }﹩ (black solid line), and a Kroupa initial mass function (IMF), are shown. Locations corresponding to ages of 0.1, 0.5, 1, 3, 6, and 13 Gyr are depicted with cyan triangles in each SSP. The chosen color cut separates clusters older than 3 Gyr from the younger ones for unreddened SSPs. The reddening vector with AV = 1 mag is represented by the black arrow.
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: Left panel: example of one completeness curve in the i band for the s27s34 field. The horizontal blue dashed line represents the completeness at the 50% and 90% levels. Center panel: distribution of i﹩{}_{{\mathrm{mag}}_{50}}﹩ magnitudes recovered for all of the Fornax pointings. The vertical black dashed line represents the mean value of the distribution. Right panel: completeness tests for mock sources with different Gaussian profile sizes: ﹩0\mathop{.}\limits^{^{\prime\prime} }55﹩ (black curve), ﹩1\mathop{.}\limits^{^{\prime\prime} }65﹩ (red curve), ﹩2\mathop{.}\limits^{^{\prime\prime} }75﹩ (green), and ﹩5\mathop{.}\limits^{^{\prime\prime} }5﹩ (yellow curve).
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: Contaminants estimation in the (u − i)0 vs. (g − i)0 color–color diagram. Comparison of structural parameters in the S-PLUS-s26s39 Fornax field (left panels) and in the S-PLUS-s46s27 control field (right panels). From top to bottom, we show SPREAD_MODEL × 100, CLASS_STAR, and FWHM. NTOT are all of the objects present in each FOV (small colored dots), and NSELECT are the objects that meet with the selection criteria (small colored dots into black open circles), respectively. The magenta and red lines sketch the loci of SSPs models with Z = 0.0004 and Z = 0.03, respectively. The cyan and yellow lines sketch the loci of zero-age main sequence (ZAMS) stars with Z = 0.0001 and Z = 0.04, respectively.
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: Contaminants estimation in the i0 vs. (g − i)0 CMD in three selected fields, which have high (left), medium (center), and low (right) crowding. The cloud of black small dots is all of the detections in each pointing. Blue circles are the observed stars (sources with CLASS_STAR > 0.90), green circles are the expected stars from Besançon models (A. C. Robin et al. 2003), and red circles are the BF-GCC. Red dashed line represents the bright selection limit in magnitude, which is estimated using the turnover of the GCLF (see Section 4.2).
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 − z)0 vs. (r − z)0 diagram with color bars indicating the GMM probability distribution to be red (top color bar) and blue (right color bar) GC candidates. The evolutionary loci of SSPs from G. Bruzual & S. Charlot (2003) corresponding to a Kroupa IMF with Z = 0.001 (black solid curve) and Z = 0.019 (yellow solid curve) are shown. Locations corresponding to 1, 2, 3, and 12 Gyr in each locus are indicated with different symbols (see the symbol code in the plot). The reddening vector with AV = 1 mag is represented by the black arrow.
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: i-band GCLF distribution (histogram). The red dashed line is the expected GCLF using a log-normal distribution corrected for incompleteness in magnitude. The vertical dashed lines indicate the magnitude at which the detection is 50% is complete. Poisson error bars (﹩\sqrt{N}﹩) are indicated.