adsabs/AstroCLIMB huggingface dataset:
Paper: Polarized Multiwavelength Emission from Pulsar Wind—Accretion Disk Interaction in a Transitional Millisecond Pulsar
Authors: Maria Cristina Baglio, Francesco Coti Zelati, Alessandro Di Marco, Fabio La Monaca, Alessandro Papitto, Andrew K. Hughes, Sergio Campana, David M. Russell, Diego F. Torres, Francesco Carotenuto, Stefano Covino, Domitilla de Martino, Stefano Giarratana, Sara E. Motta, Kevin Alabarta, Paolo D'Avanzo, Giulia Illiano, Marco M. Messa, Arianna Miraval Zanon, Nanda Rea
Figure caption: Normalized, background-subtracted Stokes parameters q and u for the average X-ray emission. The results are derived from the analysis of the combined data from all three DUs with no selection of the modes. The Stokes parameters were grouped into four bins with sizes of 1 keV across the 2–6 keV energy band. Each diamond represents the mean value, with error bars indicating the 1σ standard deviation. The circles give the contours of constant polarization degree while the radial lines correspond to constant polarization angle.
Paper: Orbital Modulation of Gamma Rays up to 100 TeV from LS 5039
Authors: R. Alfaro, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, J. A. García-González, H. Goksu, A. Gonzalez Muñoz, J. A. González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. U. Nisa, N. Omodei, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, E. Varela, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, S. Yun-Cárcamo, H. Zhou, C. de León
Figure caption: Maximum electron energy achievable within LS 5039 as a function of the acceleration efficiency (left η = 1, right η = 10) and of the magnetic field, B in Gauss (x-axis), and of the distance from the companion star, ﹩{d}_{13}=\tfrac{d}{{10}^{13}\,\mathrm{cm}}﹩ (y-axis).
Paper: Orbital Modulation of Gamma Rays up to 100 TeV from LS 5039
Authors: R. Alfaro, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, J. A. García-González, H. Goksu, A. Gonzalez Muñoz, J. A. González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. U. Nisa, N. Omodei, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, E. Varela, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, S. Yun-Cárcamo, H. Zhou, C. de León
Figure caption: HAWC significance map of the LS 5039 region. The dashed box indicates the ROI for this work. White labels mark sources resolved in this analysis; light green labels indicate the known astrophysical sources inside the ROI, with LS 5039 highlighted in bold text; cyan labels show measurements from other observatories. Significance contours start at 20σ, increasing by 10σ per line. Upper right: zoomed-in HAWC significance map around LS 5039 after background sources subtraction (see Appendix C, Table 2), showing an 11σ hotspot at LS 5039’s known location.
Paper: Orbital Modulation of Gamma Rays up to 100 TeV from LS 5039
Authors: R. Alfaro, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, J. A. García-González, H. Goksu, A. Gonzalez Muñoz, J. A. González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, S. Kaufmann, D. Kieda, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. U. Nisa, N. Omodei, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, E. Varela, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, S. Yun-Cárcamo, H. Zhou, C. de León
Figure caption: The spectral energy distribution of LS 5039 at inferior conjunction (red) and superior conjunction (blue). The gray and yellow flux points are plotted from a previous H.E.S.S. study (F. Aharonian et al. 2006a).
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Residual maps of TWA 7 in F200W scaled between −0.5 and 0.5 MJy sr−1. Top: red contours represent a surface brightness of 0.12 MJy sr−1 and blue contours represent a surface brightness of −0.12 MJy sr−1 in F200W to highlight the positive and negative residuals that remain after the disk model subtraction. The lower left dashed line represents the location of the dust clump as observed by NIRCam. Bottom: contours represent a surface brightness of 7 and 20 μJy arcsec−2 (0.30 and 0.85 MJy sr−1) in the model-subtracted SPHERE data to highlight the location of the spiral arms and dust clump (B. Ren et al. 2021). The lower left dashed lines represent the location of the dust clump as observed by NIRCam (transparent) and SPHERE (opaque), while the curved dashed line just south of the star represents the location of the spiral arm as observed with SPHERE. We label the residuals similar to B. Ren et al. (2021), where S1 and S2 are the south and north spiral arms observed with SPHERE and Clump refers to the southeast dust clump.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Top left: MCRDI reduction of TWA 7 in the F200W filter. Top right: the same reduction as in the left panel, but deconvolved. Arrows and labels point to the three ring components that make up the disk, as well as the dip in surface brightness observed in the northwest region of Ring 2. The dashed circle represents the location of the second ring component. Bottom: radial surface brightness profile of the TWA 7 disk between our convolved (light blue) and deconvolved (orange) F200W images compared to the 2017 SPHERE data (black). The three ring locations are highlighted.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Final MCRDI data reductions for TWA 7 in the F200W (left) and F444W (right) filters. Both images are rotated with north up, and the “+” represents the star location. Each tick represents 1″ (∼34 au), with a total FOV of 10″ by 10″. Additionally, the surface brightness for the F200W data is scaled linearly for <1 MJy sr−1 and is in log scale for >1 MJy sr−1 to better show the complex disk morphology.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Forward-modeling results for TWA 7 in the F200W filter (top) and the F444W filter (bottom). Left is our NIRCam observations, middle is the best-fitting forward model, and right is the resulting residual map. All images are rotated with north up, and the “+” represents the star location.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Top: azimuthal surface brightness of Ring 2 as a function of angle in degrees normalized between zero and one, although we vertically separate each profile for easier viewing. The surface brightness is measured for our F200W data, as well as the 1998 NICMOS, 2017 SPHERE, and 2019 STIS data from É. Choquet et al. (2016) and B. Ren et al. (2021). Additionally we include the best-fit cosine curves and colored dashed lines representing the measured dip location. The gray dashed lines represent the dip location measured in B. Ren et al. (2021) for reference. Bottom: year each data set was taken, versus the angular separation of the dip in degrees. The black dashed line and gray shaded region represents the fit with uncertainties to the data measured in B. Ren et al. (2021). The three colored lines represent the following scenarios; (1) no change in the dip location (solid purple), (2) a rotation of ﹩0\mathop{.}\limits^{\unicode{x000b0}}74﹩ yr−1 based on the best-fit linear model to all four data points (dashed pink), and (3) a rotation of ﹩1\mathop{.}\limits^{\unicode{x000b0}}20﹩ yr−1 based on the expected rotation of a Saturn-mass planet at ﹩\sim 1\mathop{.}\limits^{^{\prime\prime} }5﹩ (solid pink–gold). All error bars represent 1σ uncertainties.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Left: CMD with F200W − F444W versus F444W. The orange data point represents C4, while the two blue triangles represents C5 and C6, where the color measurement is a lower limit. The cyan dashed line is the measurement derived from the E. F. Linder et al. (2019) planet evolutionary models for a system with an age of 7 Myr, while the magenta dashed line is for a system with an age of 10 Myr. The gray dashed lines and shaded regions show the parameter space possible for C5 and C6 within the 1σ uncertainties. Using this plot, we can effectively rule out C4 being a planet companion, as it is significantly too blue in color. However, further investigation is warranted for C5 and C6, which only have lower limits for the color. Right: planet mass sensitivity curves for the F444W filter (top) and the F200W filter (bottom) calculated from the 5σ contrast curves. Error bars represent 3σ uncertainties. For both filters the different colors represent the results derived for a system with age = 7 Myr and 10 Myr.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Top: candidate + disk models for the F200W filter. Left is our NIRCam observations, middle left is our best-fit models, middle right is the residual maps with just the disk model subtracted, and right is the full residual maps with the disk and candidate models subtracted. The figure is zoomed in on candidate C4 (labeled), which is the only new companion candidate seen in F200W. Middle: companion + disk models for the F444W filter, including models for C4, C5, and C6 (labeled). Bottom: same as middle panel, but zoomed in within 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 to better view C5 and C6. The background star, C1, is also included in the forward-model fitting for both filters. The circles in the residual maps indicate the location of each companion.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: CMDs illustrating the extreme redness of the C6 companion (red). Gray points show JWST synthetic photometry of brown dwarfs from S. A. Beiler et al. (2024a, gray). Left: selection of Sonora Flame Skimmer models with [M/H] = +0.0, C/O = 1.0, and Kzz = 1 × 109. Right: atmospheric model tracks from Sonora Bobcat (solid circles) and ATMO2020 (dotted triangles) are compared to new Sonora Flame Skimmer models with enhanced metallicity (dashed lines). Custom models generated for this study are shown with dashed–dotted lines.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Starburst galaxy and AGN SEDs of various redshifts consistent with the flux of C6 measured at 11 μm (gray data point) and nondetections with SPHERE and ALMA (black triangles). The red data point represents the flux of C6 measured in F444W within a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 aperture, while the orange data point represents the flux of C6 measured in F444W derived from the point-source modeling.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Zoom-in view of the F200W data (left) and the model-subtracted residuals in F200W (right) around the location of C5. The green dashed contours in the left plot represent the surface brightness of the disk in F200W (between 1 and 4 MJy sr−1), while the solid multicolor contours trace the flux of C5 in F444W (between 0.13 and 0.19 MJy sr−1). The white star represents the location of the TWA 7 star.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: 5σ contrast curves for the F200W (navy) and F444W (orange) filters. The dashed lines represent 1σ deviations from the 5σ contrast curves. The orange data points represent the contrasts of the candidates, C4–C6, in the F444W filter, while the navy data point represents the contrast of the candidate, C4, in F200W. The navy triangles represents the 3σ upper limits placed on candidates C5 and C6 in F200W.
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Left: F200W observations highlighting the location of Ring 2 with the dashed gray line, as well as the location of C6 with the solid black line. Right: zoom-in view of the candidate C6 in F444W. The contours represent the planet candidate imaged at 11 μm with MIRI (A. M. Lagrange et al. 2025).