adsabs/AstroCLIMB huggingface dataset:
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: All three transit fits of AU Mic c, with the best-fit GP mean model (stellar rotation and other long-term trends) subtracted off.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: The top three panels show DES gri optical images of three SPT galaxy clusters, including SPT-CLJ0106-5943, SPT-CLJ0106-5355, and SPT-CLJ2341-5119. The white boxes show the location of the two highest-probability BCG candidates for each cluster, while the white numbers show the probability (in percentage) for each object to be a true BCG. The three examples are ranging from z = 0.35 to z = 1.00, demonstrating the ability of this method to find BCG candidates up to high redshift. The bottom three panels show the corresponding WISE images from the W1 channel for the three SPT clusters. The green boxes show the same location of the two highest-probability BCG candidates, suggesting that the BCG candidates are detectable in mid-IR.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: This figure shows a comparison of W1–W2 between AllWISE and CatWISE. The red line is the median of the difference at 0.042 mag.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: Top: W1–W2 color for each BCG candidate as a function of cluster redshift. The solid orange line shows the expected color as a function of redshift for our elliptical galaxy model using EzGal, as described in Section 3.1.1. The dashed green line shows our criterion for selecting AGNs, which is derived from the orange line, and the dotted pink line shows the cut from the previous work by Stern et al. (2012). Bottom: the W1–W2 color difference between each BCG candidate and the expected color. The dashed green line shows our selection with the residual >0.2. Every object with a residual greater than 0.2 is likely to be an AGN. The vertical dashed gray lines show the binning for the results in Figure 6. The redshift bins are defined such that each bin contains roughly the same number of systems, making for uniform counting statistics across all redshifts. The two colored stars are known BCGs in galaxy clusters with a high SFR, showing that our selection criterion does not select these starburst BCGs, while the two clusters with luminous AGNs (H 1821+643 and IRAS 09104+4109) are clearly above our criterion.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: Left: W1–W2 colors (black dots) for each BCG candidate in this sample. The solid lines show the expected color as a function of redshift using EzGal models for both a single-burst stellar population (blue) and the two-age stellar populations (orange). The single-burst models are plotted from a wide range of parameters, including two IMF (Salpeter 1955; Chabrier 2003), three formation redshifts (zf = 1.5, 2.5, and 3.5), and a span of metallicity from 0.75 to 1.0 Z⊙. To obtain the best fit, we perform a grid search between the IMF and the three formation redshifts before fitting the metallicity to minimize the chi-square. The old and young stellar models use the same parameter sets, but include an additional “young” population, which is represented by a 50 Myr old stellar population at all observed redshifts. Right: The fraction of AGN-hosting BCGs as a function of redshift for all models. The figure demonstrates that the fraction of AGN-hosting BCGs increases with redshift regardless of our choice of stellar population model.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: Residual plot similar to the bottom panel of Figure 3. The blue points are the W1–W2 color difference between each BCG candidate and the expected color. The gray squares emphasize the W1–W2 color from WISE for the sample that has been observed by Spitzer, while the green circles show the color from Spitzer, demonstrating that most of the objects we classify as AGNs have a difference of Spitzer and WISE color that is either compatible (60% of the sources have a difference of within ± 0.07 mag) or Spitzer is slightly redder (33% of the sources have a Spitzer color larger than the WISE colr by ∼0.2 mag). This means that the color and our results are not strongly impacted by WISE’s larger PSF.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: The fractions of AGN-hosting BCGs as a function of redshift. Blue points show the fractions from this work, which come from the W1–W2 color residual in the SPT sample. The size of the error bar takes the binomial uncertainty into account. Gray crosses show the fraction of points that has residuals lower than −0.2, which we consider a “noise level.” This figure demonstrates that the fraction of AGN-hosting BCG increases with redshift.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: All three panels show the fractions of AGN-hosting BCGs, similar to Figure 6. The left panel (triangles) shows the fraction when we consider only the most likely BCG for each cluster. The middle panel (dots) includes all possible BCGs with a probability higher than 20%, while the right panel (squares) includes those with a probability higher than 10%. In all scenarios, the fraction increases as a function of redshift.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: The fractions of clusters with AGN-hosting BCGs, similar to Figure 6. The blue points assume one BCG per cluster and incorporate the probability of being a BCG, estimated from Section 2.2. The empty gray dots are for clusters for which any of their potential BCGs are considered as AGNs, which is equivalent to the maximum fraction. The empty gray squares only include clusters whose BCG candidates are all considered AGNs, which is the minimum fraction. This figure shows that all of these definitions qualitatively give the same conclusion as our initial results.
Paper: The Evolution of AGN Activity in Brightest Cluster Galaxies
Authors: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, and R. D. Wilkinson
Figure caption: Comparison of the fraction of clusters with AGN-hosting BCGs to other published works. Left: Green and pink squares are the field AGN fraction from Silverman et al. (2009) and Haggard et al. (2010), respectively. The dotted gray line indicates pure luminosity evolution ∝ (1 + z)3 as suggested by Lehmer et al. (2007), while the dashed gray line shows the (1 + z)5.3 line suggested by Martini et al. (2009). The dash-dotted brown line displays the best-fit model in the form ﹩{\left(1+z\right)}^{4.1\pm 1.0}﹩. Middle: Orange diamonds show the estimated fractions of BCGs with bright AGNs (﹩{\mathrm{log}}_{10}({L}_{{\rm{X}},\mathrm{nuc}}\,[\mathrm{erg}\,{{\rm{s}}}^{-1}])\gt 42.2﹩) from Hlavacek-Larrondo et al. (2013), and open orange diamond showing the scaled version by changing the total number of clusters to the larger parent sample that Hlavacek-Larrondo et al. (2013) had drawn from because this work only focuses on highly X-ray luminous clusters (LX > 3 × 1044  erg s−1). Right: Purple points show the fraction of BCGs with an SFR > 100 M⊙ yr−1 from McDonald et al. (2016).
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Top: KLIP–RDI reduced images of the disk around AB Aur at Ks (left), 3.08 μm Ice (center), and ﹩L^{\prime} ﹩ (right). Middle: the same as the top panel, but multiplied by r2 to enhance the outer substructure. Bottom: uncertainty noise maps from the KLIP–RDI reduction of the PSF reference stars. The field of view is 3″ × 3″ with north being up and east being left. A software mask (black) of 0.″15 in radius is centered on each image. A black software mask also covers a ghost in the H2O 3.08 μm noise map NW of the central mask.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: TP map resulting from the KLIP–RDI reduction for the Ks (top), 3.08 μm Ice (center), and ﹩L^{\prime} ﹩ (bottom) filters. The left-hand column shows the true TP and the right-hand column is the azimuthally averaged TP. A value of 0 means that all flux is removed by RDI, while a value of 1 means that no flux is lost. The “point source” to the west of the ﹩L^{\prime} ﹩ TP map is an artifact in the postprocessing.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Left: the optical to far-infrared SED of AB Aur. A reddening extinction correction is applied using AV = 0.431 mag (Vioque et al. 2018), assuming a Cardelli et al. (1989) extinction law. The blue circles indicate the known observed photometry from the literature (photometry downloaded from the VizieR photometry viewer). The dark red spectra are from 1–2.46 μm, taken from the Astrophysical Research Consortium 3.5 m TripleSpec at the Astrophysical Observatory of the Smithsonian Institution. The red spectra are from the Infrared Space Observatory Short Wavelength Spectrometer (ISO/SWS; van den Ancker et al. 2000). The gold line shows the best-fit Kurucz stellar atmosphere model in the optical (T = 9772 K, ﹩\mathrm{log}{\text{}}g=4.0﹩). The thick solid black line is the best-fit MCFOST model. Right: AB Aur spectra from 2.4–5 μm, overlaid with the literature photometry (blue) and the LMIRCam H2O–Ice2 (the thin black line) and ﹩L^{\prime} ﹩ (the magenta line) filters, respectively. The synthetic photometry for each filter is shown by the corresponding colored star.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: (a) Main panel: Ks-band total intensity imagery from this work overlain with the H-band polarized intensity contours from Hashimoto et al. (2011; cyan) and Boccaletti et al. (2020; magenta). Right-hand inset: the three individual Ks-band total intensity images, with morphology that closely matches that of the H-band PI imagery, for which PSF subtraction is unnecessary, suggesting that KLIP–RDI is able to accurately recover the disk surface brightness morphology. (b) Main panel: Ks-band total intensity imagery overlain with the contours of the H2O 3.08 μm band (cyan) and L′ band (magenta). Right-hand inset: the three individual images are on equivalent scales (top to bottom: Ks, 3.08 μm, and ﹩L^{\prime} ﹩). These reveal that the observed H2O 3.08 μm morphology most closely resembles that of the Ks band. This suggests that the scattering surfaces at these two wavelengths are likely to be at similar depths in the disk surface layers. The poor qualitative and quantitative match of the ﹩L^{\prime} ﹩ morphology to the other two wavelengths suggests that the ﹩L^{\prime} ﹩ scattering surface is likely located deeper in the disk surface layer.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption:  ﹩L^{\prime} ﹩ KLIP–RDI reduced image of the disk of AB Aur overlaid with the locations of the spiral arms from Boccaletti et al. (2020) in green. The spiral arms align with the areas of brighter flux in the ﹩L^{\prime} ﹩ image, indicating that they are substructure in the disk and not artifacts from data reduction.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Radial profiles along the major (left) and minor (right) axes of the disk of AB Aur. The Ks band is shown in blue, 3.08 μm Ice is shown in black, and ﹩L^{\prime} ﹩ is shown in pink. Top: disk to star contrast of the observations as a function of distance from the central star. Middle: the surface brightness of the disk as a function of distance from the central star. Bottom: the scattered light color excess as a function of distance from the central star. Δ(Ks − H2O) is shown in green, while ﹩{\rm{\Delta }}({K}_{s}-L^{\prime} )﹩ is shown in purple.