adsabs/AstroCLIMB huggingface dataset:
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Closure-only images of source 2229+695 at 10.5 GHz for four epochs: 2019 February 19(first), 2020 December 10 (second), 2022 January 27 (third), and 2024 January 17 (fourth). These images were obtained from quad-band VLBI sessions vt9050, vo0345, vo2027, and vo4017, respectively. The circular Gaussian components determined from model fitting are shown as magenta circles. The angular distance in R.A.∗ between the peak component and the western component was estimated to be 306 ± 11 μas, 456 ± 3 μas, 641 ± 6 μas, and 743 ± 2 μas at these four epochs, respectively.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Sensitivity of the existing quad-band VLBI observations to source coordinates as a function of decl. For each source, the median absolute value of the partial derivatives of the group delays with respect to each of the two coordinates, R.A.∗ and decl., is calculated based on the actual observations of the 177 sessions and is shown by a red dot. The lower and upper bars represent the first and third quantiles of the absolute values of the partial derivatives, respectively.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Illustration of intrinsic position variations for the source 3C418 along its jet. The top panel shows the variation of its quad-band position on the sky, while the bottom panel shows the derived closure-only images at 5.5 GHz (bottom left-hand panel) and 10.5 GHz (bottom right-hand panel) from session vr2204. The ellipse in the bottom left-hand corner of the image plots shows the beam size.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Distribution of the quad-band positions of source 2229+695, with respect to its S/X position in the ICRF3, at 131 epochs. The standard deviation of the positions with respect to the weighted mean value is shown in the upper right-hand corner.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Variation of the quad-band coordinates of source 0059+581 over time. A smoothing model with one order polynomial and a time window of seven points is applied to the time series and shown as the red curve. The wrms value of the residuals with respect to this model is reported in the upper right-hand corner of each panel.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Time series of the quad-band positions of source 2229+695. Three linear segments were fitted to the R.A.∗ coordinate, while one segment was fitted to the decl. coordinate on the entire time span. The fitted segments are shown as red lines. The weighted rms residual with respect to the fitted segments that model the source motion is 0.05 mas for R.A.∗ and 0.04 mas for decl.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The 12CO J = 1–0 integrated intensity maps of the three velocity components in RCW 106 East (G333) superposed on the Herschel 160 μm continuum image (S. Molinari et al. 2010a) for the (a) −72 km s−1 MCEAST, (b) −54 km s−1 MCEAST, and (c) −42 km s−1 MCEAST. The data are smoothed to be 50″ using a kernel Gaussian function. The cross marks are positions of the massive star-forming regions in RCW 106 East (I. Bains et al. 2006). The integrated velocity range of −72 km s−1 MCEAST, −54 km s−1 MCEAST, and −42 km s−1 MCEAST is from −75 km s−1 to −65 km s−1, from −62 km s−1 to −45 km s−1, and from −45 km s−1 to −35 km s−1, respectively. The lowest contour level and interval are 10 K km s−1 and 13 K km s−1 in the panel (a), 40 K km s−1 and 40 K km s−1 in the panel (b), 15 K km s−1 and 15 K km s−1 in the panel (c).
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The 12CO J = 1–0 integrated intensity maps of the three velocity components in RCW 106 West superposed on the Herschel 160 μm continuum image (S. Molinari et al. 2010a) for the (a) −​​​​​​64 km s−1 MCWEST, (b) −54 km s−1 MCWEST, and (c) −44 km s−1 MCWEST. The data are smoothed to be 50″ using a kernel Gaussian function. The integrated velocity range of −64 km s−1 MCWEST, ​​​​​​−54 km s−1 MCWEST, and −44 km s−1 MCWEST is from −74 km s−1 to −60 km s−1, from −60 km s−1 to −49 km s−1, and from −49 km s−1 to −38 km s−1, respectively. The lowest contour level and interval are 25 K km s−1 and 25 K km s−1 in the panel (a), 15 K km s−1 and 18 K km s−1 in the panel (b), 15 K km s−1 and 16.5 K km s−1 in the panel (c).
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The CO J = 1–0 spectra in RCW 106 West at (a) ﹩(l,b)=(330\mathop{.}\limits^{^\circ }93,-0\mathop{.}\limits^{^\circ }39)﹩ and (b) ﹩(l,b)=(330\mathop{.}\limits^{^\circ }84,-0\mathop{.}\limits^{^\circ }29)﹩ obtained by Mopra. Black and blue spectra show 12CO and 13CO J = 1–0 emission, respectively. Red arrows present the three velocity components of −64 km s−1, −54 km s−1, and −44 km s−1. The black arrows show the velocity components of the Norma arm. The position of spectra in the panel (a) and (b) is the green circles of C and D in Figure 11(b), respectively. (c) The 12CO J = 1–0 longitude–velocity diagram in RCW 106 West. The integrated latitude range is from ﹩-0\mathop{.}\limits^{^\circ }60﹩ to ﹩-0\mathop{.}\limits^{^\circ }25﹩. (d) The 12CO J = 1–0 latitude-velocity diagram in RCW 106 West. The integrated longitude range is from ﹩330\mathop{.}\limits^{^\circ }6﹩ to ﹩331\mathop{.}\limits^{^\circ }2﹩. The lowest contour levels and intervals are 0.5 K degree in the panel (c). The lowest contour levels and intervals are 0.4 K degree and 0.7 K degree in the panel (d), respectively.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The CO J = 1–0 spectra in RCW 106 East at (a) ﹩(l,b)=(333\mathop{.}\limits^{^\circ }19,-0\mathop{.}\limits^{^\circ }53)﹩ and (b) ﹩(l,b)=(332\mathop{.}\limits^{^\circ }83,-0\mathop{.}\limits^{^\circ }44)﹩ obtained by Mopra. Black and blue spectra show 12CO and 13CO J = 1–0 emission, respectively. Red arrows present the three velocity components of −72 km s−1, −54 km s−1, and −​​​​​​42 km s−1. The position of spectra in the panel (a) and (b) is the green circles of A and B in Figure 11(a), respectively. (c) The 12CO J = 1–0 longitude–velocity diagram in RCW 106 East. The integrated latitude range is from ﹩-0\mathop{.}\limits^{^\circ }65﹩ to ﹩-0\mathop{.}\limits^{^\circ }15﹩. (d) The 12CO J = 1–0 latitude-velocity diagram in RCW 106 East. The integrated longitude range is from ﹩332\mathop{.}\limits^{^\circ }9﹩ to ﹩333\mathop{.}\limits^{^\circ }4﹩. The lowest contour levels and intervals are 0.4 K degree and 0.7 K degree, respectively.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The 12CO J = 1–0 integrated intensity maps of (a) the −68 km s−1 GMC and (b) −50 km s−1 GMC obtained by NANTEN2. The integrated velocity ranges of (a) and (b) are from −75 km s−1 to −60 km s−1 and from −60 km s−1 to −45 km s−1   respectively. The lowest contour and interval of the panel (a) are 20 K km s−1 and 20 K km s−1, respectively. The lowest contour and interval of the panel (b) are 30 K km s−1 and 30 K km s−1, respectively. The orange cross marks at East and West show the position of spectra in Figures 3(a) and (b), respectively.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The 12CO J = 1–0 velocity channel map obtained by NANTEN2. The cube data is smoothed to the velocity domain of nine channels by the hanning window. Red-dotted rectangles show giant molecular filaments of GMF 335.6-333.6a and GMF 335.6-333.6b.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: The 12CO J = 1–0 integrated intensity maps of (a) the −68 km s−1 GMC and (b) −50 km s−1 GMC obtained by NANTEN2 superposed on the Herschel 160 μm continuum image (S. Molinari et al. 2010a). The lowest contour and interval of the panel (a) is 20 K km s−1. The lowest contour level and interval of the panel (b) is 30 K km s−1.
Paper: Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud–Cloud Collisions
Authors: Mikito Kohno, 樹人 河野, Rin I. Yamada, 麟 山田, Kengo Tachihara, 研悟 立原, Shinji Fujita, 真司 藤田, Rei Enokiya, 玲依 榎谷, Kazuki Tokuda, 一起 徳田, Asao Habe, 朝男 羽部, Hidetoshi Sano, 栄俊 佐野, Takahiro Hayakawa, 貴敬 早川, Fumika Demachi, 史夏 出町, Takuto Ito, 拓冬 伊藤, Kisetsu Tsuge, 紀節 柘植, Atsushi Nishimura, 淳 西村, Masato I. N. Kobayashi, 将人 小林, Hiroaki Yamamoto, 宏昭 山本, Yasuo Fukui, 康雄 福井
Figure caption: Spectra for 12CO J = 1–0 obtained at (a) RCW 106 East (G333), and (b) RCW 106 West with NANTEN2. The red arrows indicate the velocity components associated with the RCW 106 GMC complex. The black arrow shows the velocity component of the Norma arm. The spectra are smoothed to the velocity domain of 9 channels by the hanning window. The position of each spectrum is shown in the upper right of each panel and the orange cross marks in Figures 5(a) and (b).
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The NIRCam F150W and F410M filter image of the Ced 110 IRS4 region in gray scale is shown, with the ALMA 1.3 mm continuum map overlaid as magenta contours. The 1.3 mm continuum maps, with robust parameters of 2.0 and 0.0, are overlaid on the wide and zoomed-in views of the NIRCam image, respectively. The contours are 3σ, 10σ, 30σ, 70σ, and 100σ, with σrobust = 2  = 14 μJy and 10σ, 30σ, 70σ, and 100​​​​​​σ with σrobust = 0  = 16 μJy. The NIRCam FWHM and the ALMA beams are shown in the lower left corner as blue and red ellipses, respectively. The scale bar in white is also shown in the lower right corner. The beam sizes and PA are given in Tables 1 and 2.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The morphology of the [Fe II] lines detected toward Ced 110 IRS4. All images are cropped to the same spatial scale of 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 × 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 and have the same color scale. The ALMA 1.3 mm contours are shown in lime. The scale bar corresponding to 100 au is shown in the lower right corner. The MIRI MRS FWHM based on D. D. Law et al. (2023) is shown in the lower left corner as a blue circle, and the ALMA beam is shown in red. We also show in cyan apertures (radius = MIRI MRS FWHM) used to extract line flux from the two protostars.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The NIRCam F150W and F410M filter image of the Ced 110 IRS4 region in gray scale. The NIRCam FWHM is shown in the lower left corner in blue. The scale bar in white is also shown in the lower right corner. The beam sizes are given in Table 2. The arc-like structure is marked with a magenta line, and the dark band is marked with a cyan line. The same intensity scaling is followed in Figure 2 for the NIRCam observations.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The NIRCam F150W filter image of the Ced 110 IRS4 region, with the ALMA (SB) CO isotopologue integrated intensity image overlaid as magenta contours. The contours for 12CO and 13CO are 15%, 30%, 50%, 70%, 90%, and 99%  × Fmax, where Fmax for 12CO is 0.36 Jy beam−1 km s−1; Fmax for 13CO is 0.17 Jy beam−1 km s−1. The contours for C18O are 30%, 50%, 70%, 90%, and 99%  × Fmax, where Fmax for C18O is 0.07 Jy beam−1 km s−1. The NIRCam FWHM and the ALMA beams are shown in the lower left corner as blue and red ellipses, respectively. The beam sizes and PA are given in Tables 1 and 2. All NIRCam images have the same intensity scale.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The morphology of the atomic FS lines detected toward Ced 110 IRS4. All images are cropped to the same spatial scale of 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 × 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 and have the same color scale. The ALMA 1.3 mm contours are shown in lime. The scale bar corresponding to 100 au is shown in the lower right corner. The MIRI MRS FWHM based on D. D. Law et al. (2023) is shown in the lower left corner as a blue circle, and the ALMA beam is shown in red. We also show in cyan apertures (radius = MIRI MRS FWHM) used to extract line flux from the two protostars.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: (a) The horizontal slices in green marked on top of the jet traced in [Fe II] at 5.34 μm. The white circle represents the protostellar position. The cyan dashed line marks the jet axis, which is perpendicular to the disk as traced in ALMA dust continuum. (b) The observed (in red) and deconvolved (in blue) jet width (FWHM) of the jet as a function of distance from the central protostar. The negative distance corresponds to the northern side, and the positive distance corresponds to the southern side.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The NIRCam F150W filter image of the Ced 110 IRS4 region, with the ALMA (SBLB) CO isotopologue integrated intensity image overlaid as magenta contours. The contours for are 15%, 30%, 50%, 70%, 90%, and 99% × Fmax, where Fmax for 12CO is 150 mJy beam−1 km s−1; Fmax for 13CO is 60 mJy beam−1 km s−1, and Fmax for C18O is 30 mJy beam−1 km s−1. The NIRCam FWHM and the ALMA beams are shown in the lower left corner as blue and red ellipses, respectively. The beam sizes and PA are given in Tables 1 and 2. All NIRCam images have the same intensity scale.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The atomic jet has traced in [Fe II] at 5.34 μm and [Ne II] at 12.81 μm, with NIRCam F150W emission overlaid on top in magenta. The MIRI FWHM based on D. D. Law et al. (2023) is shown in the lower left corner as a blue circle, while the NIRCam FWHM is shown as a red circle.
Paper: An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4
Authors: Mayank Narang, Nagayoshi Ohashi, John J. Tobin, M. K. McClure, Jes K. Jørgensen, Jinshi Sai (Insa Choi)
Figure caption: The MIRI MRS continuum image of the Ced 110 IRS4 region in gray scale. The ALMA 1.3 mm position for Ced 110 IRS4A is shown as a red circle, and that for IRS4B is shown as a yellow circle. The scale bar corresponding to 100 au is shown in the lower right corner. The MIRI FWHM based on D. D. Law et al. (2023) is shown in the lower left corner as a blue circle.
Paper: Use the 4S (Signal-Safe Speckle Subtraction): Explainable Machine Learning Reveals the Giant Exoplanet AF Lep b in High-contrast Imaging Data from 2011
Authors: Markus J. Bonse, Timothy D. Gebhard, Felix A. Dannert, Olivier Absil, Faustine Cantalloube, Valentin Christiaens, Gabriele Cugno, Emily O. Garvin, Jean Hayoz, Markus Kasper, Elisabeth Matthews, Bernhard Schölkopf, Sascha P. Quanz
Figure caption: Top row: illustration of how PCA is applied to ADI data in HCI. The planetary signal is shown in blue, while the stellar speckle noise is represented by the red splash. Details about the steps (① to ⑤) are given in the text. Bottom row: examples of the first five principal components are shown, estimated for data set #5 (HD 22049) in Table 1. Further details on the data are given in Section 5. The first components of PCA are often interpretable. For example, u1 in the given example models the overall brightness variations of the postcoronagraphic PSF. The components u2 and u3 represent horizontal and vertical variations caused by small errors in the centering of the star behind the coronagraph.
Paper: Signatures of Atmospheric Mass Loss and Planet Migration in the Time Evolution of Short-period Transiting Exoplanets
Authors: Rachel B. Fernandes, Galen J. Bergsten, Gijs D. Mulders, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Steven Giacalone, Jessie L. Christiansen, James G. Rogers, Akash Gupta, Rebekah I. Dawson, Tommi T. Koskinen, Kiersten M. Boley, Jason L. Curtis, Katia Cunha, Eric E. Mamajek, Sabina Sagynbayeva, Sakhee S. Bhure, David R. Ciardi, Preethi R. Karpoor, Kyle A. Pearson, Jon K. Zink, Gregory A. Feiden
Figure caption: Normalized density distributions of stellar properties such as stellar mass (top left), radius (top right), effective temperature (bottom left), and Gaia magnitude (bottom right) for host stars from Kepler (black solid lines), J. L. Christiansen et al.’s (2023) K2 Praesepe (black dashed lines), and TESS (pink and blue shaded regions for young and intermediate-age stars, respectively).
Paper: Signatures of Atmospheric Mass Loss and Planet Migration in the Time Evolution of Short-period Transiting Exoplanets
Authors: Rachel B. Fernandes, Galen J. Bergsten, Gijs D. Mulders, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Steven Giacalone, Jessie L. Christiansen, James G. Rogers, Akash Gupta, Rebekah I. Dawson, Tommi T. Koskinen, Kiersten M. Boley, Jason L. Curtis, Katia Cunha, Eric E. Mamajek, Sabina Sagynbayeva, Sakhee S. Bhure, David R. Ciardi, Preethi R. Karpoor, Kyle A. Pearson, Jon K. Zink, Gregory A. Feiden
Figure caption: Top: overall detection efficiency of pterodactyls in ﹩\frac{{R}_{\,\rm{p}\,}}{{R}_{\star }}﹩ space for the full sample. Center: detection efficiency of the FGK stars in our sample. Bottom: completeness of the FGK sample, which combines the detection efficiency with the geometric transit probability. The black box denotes the bin over which the intrinsic occurrence rates were calculated, i.e., sub-Neptunes and Neptunes (1.8–10 R⊕) within 12 days.
Paper: Signatures of Atmospheric Mass Loss and Planet Migration in the Time Evolution of Short-period Transiting Exoplanets
Authors: Rachel B. Fernandes, Galen J. Bergsten, Gijs D. Mulders, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Steven Giacalone, Jessie L. Christiansen, James G. Rogers, Akash Gupta, Rebekah I. Dawson, Tommi T. Koskinen, Kiersten M. Boley, Jason L. Curtis, Katia Cunha, Eric E. Mamajek, Sabina Sagynbayeva, Sakhee S. Bhure, David R. Ciardi, Preethi R. Karpoor, Kyle A. Pearson, Jon K. Zink, Gregory A. Feiden
Figure caption: Comparison of the number of planets per star (F0), period (α), and radius (β) exponents across the different age bins.
Paper: Signatures of Atmospheric Mass Loss and Planet Migration in the Time Evolution of Short-period Transiting Exoplanets
Authors: Rachel B. Fernandes, Galen J. Bergsten, Gijs D. Mulders, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Steven Giacalone, Jessie L. Christiansen, James G. Rogers, Akash Gupta, Rebekah I. Dawson, Tommi T. Koskinen, Kiersten M. Boley, Jason L. Curtis, Katia Cunha, Eric E. Mamajek, Sabina Sagynbayeva, Sakhee S. Bhure, David R. Ciardi, Preethi R. Karpoor, Kyle A. Pearson, Jon K. Zink, Gregory A. Feiden
Figure caption: Comparison of the Kepler’s inverse detection efficiency values (circles) and our best-fit occurrence models (lines) in orbital period and radius space, respectively, (top) with our entire sample (10–1000 Myr) and (bottom) split into young (10–100 Myr) and intermediate (100–1000 Myr).