adsabs/AstroCLIMB huggingface dataset:
Paper: A Catalog of Distance Determinations for the LAMOST DR8 K Giants in the Galactic Halo
Authors: Lan Zhang, Xiang-Xiang Xue, Chengqun Yang, Feilu Wang, Hans-Walter Rix, Gang Zhao, Chao Liu
Figure caption: Calibration results. The upper panels show adjusted PS1 photometry. Red dashed lines are diagonals. The lower panels present PDFs of Δ m  after calibration. The mean values and 68% intervals are shown in red lines and shades, respectively.
Paper: A Catalog of Distance Determinations for the LAMOST DR8 K Giants in the Galactic Halo
Authors: Lan Zhang, Xiang-Xiang Xue, Chengqun Yang, Feilu Wang, Hans-Walter Rix, Gang Zhao, Chao Liu
Figure caption: Number density distributions of K-giant sample in the color–magnitude and color–metallicity plane. In the bottom panel, red and dark blue points represent possible RC and HB stars, respectively.
Paper: A Catalog of Distance Determinations for the LAMOST DR8 K Giants in the Galactic Halo
Authors: Lan Zhang, Xiang-Xiang Xue, Chengqun Yang, Feilu Wang, Hans-Walter Rix, Gang Zhao, Chao Liu
Figure caption: The number and σ D/D distributions in R GC–∣z∣ plane for the halo K giants. The stars can trace as far as R GC = 125 kpc with good precisions.
Paper: A Catalog of Distance Determinations for the LAMOST DR8 K Giants in the Galactic Halo
Authors: Lan Zhang, Xiang-Xiang Xue, Chengqun Yang, Feilu Wang, Hans-Walter Rix, Gang Zhao, Chao Liu
Figure caption: Our distances of good estimates (σ D/D < 0.15) compare with parallaxes whose relative errors σ  ϖ /ϖ < 0.1 from Gaia EDR3. Red dashed lines are diagonals.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward U Ant, imaged with GALEX. The large white dashed circle, with radius of 175″, is a fit to the estimated radial location of the termination shock in the astrosphere, seen to the west of U Ant. The smaller dashed circle, with radius of 105″, marks the location of an intensity peak in the radial intensity cut in Figure 6. The small white dashed circle, with radius of (42″) shows the location of the detached shell seen in the far-IR by Cox et al. (2012). All circles are centered on the star’s location (black cross). Vector shows the star’s proper motion of 27.5 mas yr−1 at PA = 296°, magnified by a factor of 104. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward V Hya, imaged with GALEX. In panel (a) black cross shows the location of the star, and vector shows the star’s proper motion of 12.9 mas yr−1 at PA = 315°, magnified by a factor of 104. In panel (b), dashed-dotted white elliptical arcs (dashed black elliptical arc) delineate extended regions of FUV emission that are likely associated with the blueshifted (redshifted) large parabolic outflows seen in CO emission by Sahai et al. (2022). Excess FUV emission (over the average sky background) is seen near the transverse structure labeled T. North is up and east is to the left. The scalebar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward EY Hya, imaged with GALEX. The large white dashed circle, with radius of 130″, delineates the radial extent of the termination shock in the astrosphere, west of EY Hya. Two long filamentary structures that comprise the tail region of the astrosphere are labeled T1 and T2. The emission in region labeled A is due to an imperfectly subtracted, very bright point source located at an offset of 275″ (at PA = 25°) from EY Hya. The black cross shows the star’s location. Vector shows the star’s proper motion of 9.5 mas yr−1 at PA = 261°, magnified by a factor of 104. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward R LMi, imaged with GALEX. The large white dashed circle, with radius of 295″, delineates the radial extent of the termination shock in the astrosphere; black cross shows location of the star. Vector shows the star’s proper motion of 6.9 mas yr−1 at PA = 122°, magnified by a factor of 104. Region A (magenta circle) shows local environment around two point sources that could not be removed. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around U Ant, averaged over an azimuthal wedge with its apex centered on the star and spanning the range from PA = −60° to −140°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: The FUV emission toward RT Vir, imaged with GALEX. The white dashed circle, with radius of 65″, delineates the termination shock in the astrosphere, east of the star (black cross). Vector shows the star’s proper motion of 52.6 mas yr−1 at PA = 103°, magnified by a factor of 104. Region A (magenta ellipse) shows a locally bright region near the end of the astrosphere tail. North is up and east is to the left. The scale bar shows intensity in cps pix−1.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around R LMi, averaged over an azimuthal wedge with its apex centered on the star and spanning a 320° angular range around PA = 120°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around EY Hya, averaged over an azimuthal wedge with its apex centered on the star and spanning the range from PA = −60° to −140°. The average surrounding sky intensity has been subtracted from the cut.
Paper: Faint but Not Forgotten. I. First Results from a Search for Astrospheres around AGB Stars in the Far-ultraviolet
Authors: Raghvendra Sahai, Benjamin Stenger
Figure caption: Radial intensity cut of the FUV emission around V Hya, averaged over an azimuthal wedge with its apex centered on the star and spanning the range from PA = −100° to −80°. The average surrounding sky intensity has been subtracted from the cut.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: LS periodograms for the observed RVs and spectral indices (ΔFWHM and ΔBIS) extracted from the IRD spectra. In each panel, the vertical dashed line represents the orbital period of K2-415b. The three horizontal lines correspond to the FAPs of 5%, 1%, and 0.1% from the bottom, respectively. The second panel from the top shows the LS power for the RV residuals after subtracting the best-fit orbit of K2-415b.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Mass–radius diagram for well-characterized transiting planets, taken from the TEPcat catalog (Southworth 2011). K2-415b, planets around the low-mass stars (0.1 M ⊙ < M ⋆ < 0.3 M ⊙), and TRAPPIST-1 planets are plotted by the red square, dark blue circles, and purple circles, respectively. Theoretical curves are drawn using the models by Zeng et al. (2016, 2019), in which an equilibrium temperature of 400 K was assumed.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Folded K2 (panel (a)) and TESS (panel (b)) transit light curves of K2-415b, for which a linear ephemeris is assumed. In both panels, red solid lines indicate the best-fit transit model (the e-prior fit) for the observed data, and flux residuals from the model are plotted at the bottom. For panel (a), K2's long cadence is taken into account in drawing the best-fit theoretical curve, and the original transit model before binning is shown by the cyan dashed line in the same panel.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Observed RVs (top) as well as the activity indicators (middle and bottom panels) measured from the IRD spectra. The red solid lines indicate the multidimensional GP regressions to the observed quantities using the quasi-periodic GP kernel.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Phase-folded RV curve after subtracting the correlated-noise component via the GP regression. The red solid line represents the best-fit Keplerian orbit of K2-415b, and the bottom panel plots the residuals from the best-fit orbit.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Low-resolution optical spectrum of K2-415 obtained by LAMOST (Luo et al. 2015). The inset displays a zoom-in around Hα (the red vertical line).
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Residuals from the linear ephemeris (a constant period) for K2-415b’s transit times for the K2 (top) and TESS (bottom) data.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Light curves of K2-415 obtained by K2 (top; K2SFF) and TESS (bottom; PDC-SAP). Those data were taken at long (≈29 minutes) and short (2 minutes) cadences for K2 and TESS light curves, respectively. The red solid line in each panel represents the GP regression to the observed light curve (see Section 4.4).
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: LS periodograms for the K2 (top) and TESS (bottom) light curves. The window function for each light curve is plotted by the dashed line. The secondary peak at ≈2 days represents the harmonics of the rotation period.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Sensitivity plot (5σ contrast curve) for K2-415 in the ﹩{K}^{{\prime} }﹩ band, based on the combined IRCS image. The inset shows a zoomed-in image of the target with an FoV of 4″ × 4″.
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: BLS transit signal detections for the K2 (top) and TESS (bottom) light curves. The red dashed line represents the orbital period of K2-415b (4.02 days).
Paper: An Earth-sized Planet around an M5 Dwarf Star at 22 pc
Authors: Teruyuki Hirano, Fei Dai, John H. Livingston, Sascha Grziwa, Kristine W. F. Lam, Yui Kasagi, Norio Narita, Hiroyuki Tako Ishikawa, Kohei Miyakawa, Luisa M. Serrano, Yuji Matsumoto, Eiichiro Kokubo, Tadahiro Kimura, Masahiro Ikoma, Joshua N. Winn, John P. Wisniewski, Hiroki Harakawa, Huan-Yu Teng, William D. Cochran, Akihiko Fukui, Davide Gandolfi, Eike W. Guenther, Yasunori Hori, Kai Ikuta, Kiyoe Kawauchi, Emil Knudstrup, Judith Korth, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Rafael Luque, Mayuko Mori, Jun Nishikawa, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Carina M. Persson, Seth Redfield, Eugene Serabyn, Alexis M. S. Smith, Aoi Takahashi, Takuya Takarada, Akitoshi Ueda, Vincent Van Eylen, Sébastien Vievard, Motohide Tamura, Bun'ei Sato
Figure caption: Sensitivity plots of K2-415, based on the speckle observations by NESSI. The two insets display the reconstructed images of K2-415 in the 562 nm (left) and 832 nm (right) bands.
Paper: ODNet: A Convolutional Neural Network for Asteroid Occultation Detection
Authors: Dorian Cazeneuve, Franck Marchis, Guillaume Blaclard, Paul A. Dalba, Victor Martin, Joe Asencio
Figure caption: A simulated stack (bottom) made of 20 snippets including a occultation lasting five frames. A stack (top) based on a recorded occultation observed on 2021 May 27 with the disappearance of the star over eight frames. Those stacks are part of the sequences input to ODNet.
Paper: ODNet: A Convolutional Neural Network for Asteroid Occultation Detection
Authors: Dorian Cazeneuve, Franck Marchis, Guillaume Blaclard, Paul A. Dalba, Victor Martin, Joe Asencio
Figure caption: Visualization of the process from a raw picture to a Gaussian-blurred frame to an AFD-identified frame with a coordinate grid of the RaDec in degrees and the stars selected for study. From left to right: 1-Raw frame 2-Blurred and Post AFD frame. The display for the left image was adjusted so the low-level signal, the faint stars and background noise, is visible.
Paper: ODNet: A Convolutional Neural Network for Asteroid Occultation Detection
Authors: Dorian Cazeneuve, Franck Marchis, Guillaume Blaclard, Paul A. Dalba, Victor Martin, Joe Asencio
Figure caption: Algorithm to create a random artificial star snippet as part of the training set (left) and comparison with TYC 6812-00410-1 as seen with an eVscope (right). Display is at the same scale for both frame for comparisons.
Paper: ODNet: A Convolutional Neural Network for Asteroid Occultation Detection
Authors: Dorian Cazeneuve, Franck Marchis, Guillaume Blaclard, Paul A. Dalba, Victor Martin, Joe Asencio
Figure caption: Detection of an occultation using the legacy method.