adsabs/AstroCLIMB huggingface dataset:
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: In the top, Hα, Hβ, [S II], [O III], and [N II] line flux (10−17 erg s−1 cm−2) and line-ratio maps of NGC 3182 are presented. In the bottom, we present emission-line-ratio diagrams and maps for [O III]5007/Hβ vs. [N II]6583/Hα and [O III]5007/Hβ vs. [S II]6731/Hα color coded by ionization source. The representative uncertainties are shown bottom right corner of each panel. Lines in the diagrams are from Kauffmann et al. (2003) and Sharp & Bland-Hawthorn (2010), respectively, to separate star forming, the AGN, and LINERs. Circles are the same as in Figure 4.
Paper: The Origin of the Nuclear Star-forming Ring in NGC 3182
Authors: Mina Pak, Joon Hyeop Lee, Hyunjin Jeong, Woong-Seob Jeong
Figure caption: The maps (left) and profiles (right) of the specific star formation rate (top) and gas metallicity (bottom) with corresponding uncertainties. The radial profiles are obtained from the isophotal ellipses using the IRAF/ELLIPSE task (Jedrzejewski 1987). The vertical lines distinguish the region of the star-forming ring. The error bars for log SFR and log SFR are shown but their sizes are smaller than the symbol size.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The evolutionary tracks of ELM WDs in ﹩\mathrm{log}\ g-{T}_{\mathrm{eff}}﹩ plane. Theses tracks have the same initial donor masses (1.2M ⊙) and accretor masses (1.1M ⊙). The standard evolutionary models of ELM WDs are shown in black solid lines with ELM masses of 0.16–0.21M ⊙ in a step of 0.01M ⊙ from right to left. The cross symbols denote the end of mass transfer (MT) and the start of the contraction phase. Stars between the end of MT and the beginning of WD cooling track, generally referred as pre-ELMs, have nearly constant luminosity, decreasing radius and increasing temperature, and a lifetime of ≈1 Gyr depending on their masses. The red lines are for the models with considering the pulsar evaporation effects. The models of f = 0.1 are shown in the red dotted lines, where the ELMs have masses of 0.13, 0.14, 0.15M ⊙ from right to left. The models of f = 0.2 are shown in the red dashed lines, where the ELMs have masses of 0.11, 0.12, 0.13M ⊙ from right to left. J2240 here adopts T eff = 7360 ± 150 K and log g = 4.43 ± 0.05.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: Light-curve fitting of ZTF g, r, and i bands, from top to bottom, respectively. The gray points in the upper panel denote ZTF magnitudes, and the curves are models calculated with Wilson–Devinney code, with color from red to blue denote inclination increasing from 60° to 90°. All the solid curve is fixed with a white-dwarf companion of 18,000 K. The fitting residuals are plotted in each lower panel, with a standard variation of ≈2.7%. To illustrate eclipse of white dwarf occultation in the light curve, models with white dwarfs of 12,000 K, 22,000 K, and 30,000 K are plotted with the dotted, the dot dash and the dashed line, respectively, and enlarged in the inset of each plot, while the inclination is fixed at 90°.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The bootstrapping sampling results upon ZTF g, r, and i light curves, using the Wilson–Devinney code. Diagonal elements show the probability distribution of each parameter, with percentiles of 16%, 50%, and 84%, denoted by vertical lines. Note star 1 denotes the visible component, while star 2 denotes the invisible compact component. The uncertainties of inclination, distance, extinction, gravity darkening, etc, are all taken into consideration. See text for more details.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: The SED fitting of J2240 alike Figure 5 with additional white-dwarf component. The Koester WD model (Koester 2010) is used. The green line denote the error of the observations. The model parameters of the visible component are T eff = 7320 K, log g = 4.43 and [Fe/H] = 0.08, and the E(B − V) is 0.055. The WD component is chosen to have T eff = 18,000 K, log g = 7.5 and radius ≈0.009R ⊙. The flux contributions of the white dwarf in the optical bands are ∼1%.
Paper: ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Hailong Yuan (袁海龙), Zhenwei Li (李振威), Zhongrui Bai (白仲瑞), Yiqiao Dong (董义乔), Mengxin Wang (汪梦欣), Sicheng Yu (余思成), Xuefei Chen (陈雪飞), Yongheng Zhao (赵永恒), Yaoquan Chu (褚耀泉), Haotong Zhang (张昊彤)
Figure caption: Results of sinusoidal RV fitting using MCMC technique with the eccentricity fixed to 0. The returned K1 is 318.5 ± 3.3 km s−1 and V0 is −68.6 ± 2.6 km s−1.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Eccentricity vs. semimajor axis for all confirmed planets (obtained from the NASA Exoplanet Archive 2022 February 13) with M p < 13 M J. The vertical coordinate is scaled to e 2 to emphasize noncircular planets. Shaded areas highlight different formation scenarios. Planets in the gray region are on the path of high-eccentricity migration, with a final semimajor axis between 0.034 and 0.1 au. The upper and lower bounds of this region are set by the Roche limit and the circularization timescale, respectively. Disk migration, expected to only marginally excite orbital eccentricity, is shown as the red shaded region. Finally, in situ formation, with eccentricity excited by, e.g., planet–planet scattering, is shown as the blue shaded area. Transiting vs. nontransiting planets are labeled in yellow and blue symbols, respectively. Circles are representing larger (R p > 6 R ⊕ and/or M p >  100 M ⊕) planets, and diamonds are representing smaller planets (R p < 6 R ⊕ and/or M p <  100 M ⊕). Only planets with e ≥ 0.2 and with uncertainties on e smaller than 50% of the measured e or planets with e < 0.2 and with uncertainties less than 0.2 are shown.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Top: GLS periodogram of TOI-4562’s photometry from TESS for the first (2018–2019; red line) and third (2020–2021; blue line) year of data. The identified stellar rotation period (P ⋆ = ﹩{3.86}_{-0.08}^{+0.05}﹩) and the first harmonic (P ⋆/2) are shown with the vertical brown lines, with the surrounding shaded areas representing uncertainties. Middle: GLS periodogram of ASAS-SN’s photometry gathered between 2018 and 2021 (orange line). The identified stellar rotation period (P ⋆ = 3.84 ± 0.02) and the first harmonic (P ⋆/2) are shown as the vertical brown lines with their respective uncertainties (shaded area). Bottom: Periodogram on the 4 yr (2008–2012) of WASP data yielding P ⋆ estimates between 3.74 and 3.84, depending on the considered year. In all three periodograms, we notice a strong peak multiplicity around 3.9 days that could be associated with stellar surface features tracing differential rotation.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Youth indicators for TOI-4562. Top: the rotation period of TOI-4562 compared to the distribution of stars within known associations and clusters, including the Pleiades (Rebull et al. 2016), MELANGE-1 (Tofflemire et al. 2021), Group X (Messina et al. 2022; Newton et al. 2022), Praesepe and Hyades (Douglas et al. 2016, 2019), NGC 6811 (Curtis et al. 2019), and NGC 6819 (Meibom et al. 2015). Bottom: equivalent width of the lithium doublet at 6707.76 and 6707.91 Å for TOI-4562 (black star) and stars in the Praesepe (orange circles; Cummings et al. 2017), Group X (green diamonds; Newton et al. 2022), and Pleiades (blue circles; Bouvier et al. 2018) clusters. TOI-4562 lies at an age comparable to the Hyades and Praesepe.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Young gas giants can help constrain the cooling and contraction models. To date, TOI-4562b is only the fourth Jovian planet younger than 500 Myr to have both its mass and radius measured. The mass–radius of TOI-4562b is plotted in orange alongside the planets in the V1298 Tau (David et al. 2019a; Suárez Mascareño et al. 2022) and TOI-1268 (Dong et al. 2022; Šubjak et al. 2022) systems. Unlike others, TOI-4562b sits along the isochrone tracks that model the contraction of young planets (Linder et al. 2019). The mass–radius distribution of other known planets are shown with a density plot in blue in the background.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Posterior distributions for TOI-4562 b’s orbital eccentricity (e) and argument at periapse (ω). The gray distribution was obtained from comparing ρ ⋆ obtained from an SED fit and ρ circ resulting from a fit of only the photometric data (TESS + LCO-SAAO) with an imposed circular orbit. The red and yellow posterior distributions, respectively, results from a photometric data + SED fit and the complete model including the radial velocities. .
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Top: high-resolution image of TOI-4562 obtained with the Zorro camera attached to the 8.1 m Gemini South telescope. The blue and red curves show difference in magnitude as a function of orbital separation from TOI-4562 obtained at wavelengths of, respectively, 562 and 832 nm. The inset plot shows the reconstructed image at 832 nm where no companion is detected. Bottom: SOAR HRCam high-resolution imaging of TOI-4562. The difference in magnitude as a function of orbital separation from TOI-4562 is shown by the black curve and the autocorrelation function on the inset image. There is no sign of a stellar-sized companion to TOI-4562.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Top: 2 yr radial-velocity time series of TOI-4562 obtained with the CHIRON spectrograph (brown circles) with the associated error bars. The Keplerian orbit fit from our global modeling is shown by a red line. Transits are highlighted in light brown. Bottom: phase-folded RVs (brown circles) with the Keplerian orbit best fits shown by a red line.
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: SED of TOI-4562 b. Red points are the observed magnitudes in different wavelength bands (labeled with corresponding letters) corrected from interstellar reddening. Predicted magnitudes from the isochrone part of our global model are shown as gray open squares. The gray line is a theoretical spectra for a star with T eff = 6000 K, log g = 4.5 dex, and [M/H] = 0 (adopted from Coelho 2014).
Paper: TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star
Authors: Alexis Heitzmann, George Zhou, Samuel N. Quinn, Chelsea X. Huang, Jiayin Dong, L. G. Bouma, Rebekah I. Dawson, Stephen C. Marsden, Duncan Wright, Pascal Petit, Karen A. Collins, Khalid Barkaoui, Robert A. Wittenmyer, Edward Gillen, Rafael Brahm, Melissa Hobson, Coel Hellier, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Steve B. Howell, Crystal L. Gnilka, Colin Littlefield, David W. Latham, Jack J. Lissauer, Elisabeth R. Newton, Daniel M. Krolikowski, Ronan Kerr, Rayna Rampalli, Stephanie T. Douglas, Nora L. Eisner, Nathalie Guedj, Guoyou Sun, Martin Smit, Marc Huten, Thorsten Eschweiler, Lyu Abe, Tristan Guillot, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Eric B. Ting, Joshua N. Winn, David R. Ciardi, Andrew M. Vanderburg, Christopher J. Burke, David R. Rodriguez, Tansu Daylan
Figure caption: Two-dimensional orbit of TOI-4562b (yellow solid line) compared with Mercury (red dashed line), Venus (purple dashed line), Earth (blue dashed line), and Mars (orange dashed line).
Paper: Identification of Galaxy Shreds in Large Photometric Catalogs Using Convolutional Neural Networks
Authors: Enrico M. Di Teodoro, J. E. G. Peek, John F. Wu
Figure caption: A schematic of the architecture of the convolutional neural network used in this work. Our CNN has 10 layers, including eight 2D convolutional layers (red boxes) and two fully connected layers (blue tall boxes), with approximately 10.6M parameters. Max pooling and dropout operations are denoted as green and blue boxes, respectively. In convolutional layers, we indicate the size of the 2D windows and the number of output filters. In pooling stages, we also write the size of downsampling. Activation functions are indicated in the circles (R for ReLU and S for softmax function).
Paper: Identification of Galaxy Shreds in Large Photometric Catalogs Using Convolutional Neural Networks
Authors: Enrico M. Di Teodoro, J. E. G. Peek, John F. Wu
Figure caption: Photometric sources around the spiral galaxy UGCA 021. In all panels, we show a color image in g-r-z band from the Legacy surveys. In the left panel, we show all sources in the Legacy DR9 catalog; the middle and right panels show sources in Legacy and SDSS DR17 catalogs, respectively, after some cleaning using stricter selection criteria, similar to those described in Section 3.1. In the middle and right panels, galaxy shreds are highlighted in yellow, while genuine galaxy sources in red. The only NSA spectroscopically confirmed source in this field is the galaxy UGCA 021. Images have 512 × 512 pixels with a pixel size of 0.″262. The white-dashed square in the right panel is an example of a 128 × 128 pixel image used by our CNN.
Paper: Identification of Galaxy Shreds in Large Photometric Catalogs Using Convolutional Neural Networks
Authors: Enrico M. Di Teodoro, J. E. G. Peek, John F. Wu
Figure caption: Binary classification of sources into either a galaxy or a shred using the CNN of Figure 2. The left group of panels shows a random sample of targets identified as genuine galaxies, the right group of panels a random sample of targets classified as galaxy shreds. The source in a red frame highlights a (possibly) wrong classification, i.e., a galaxy likely mislabelled as a shred by the CNN.
Paper: Identification of Galaxy Shreds in Large Photometric Catalogs Using Convolutional Neural Networks
Authors: Enrico M. Di Teodoro, J. E. G. Peek, John F. Wu
Figure caption: The receiving operator characteristic (ROC) curve for our CNN model. Black thin lines denote the five cross-validation folds used, while the mean result is shown as a thick red line. The AUC for our model is 0.985. The dashed gray line shows the baseline for a random guess (AUC = 0.5).
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption:  Top: periodogram of RX J2117.1+3412. Low-frequency signals of an eclipsing binary (orange) and high-frequency signals from stellar pulsations (blue) fit with Pyriod are marked. Middle: heatmaps for low-frequency (left) and high-frequency (right) signals. These two different types of signal clearly originate from different positions on the sky. These heatmaps are a result of summing the individual amplitude heatmaps for each frequency and dividing by the square root of the sum of the squared error heatmaps. The gray points indicate the positions of Gaia DR2 sources brighter than G = 18 mag in the field. Bottom: light curves extracted from the single hottest pixels in each heatmap (marked with a red border in the heatmaps). The binary eclipse signature is confirmed to be much more pronounced in the light curve extracted away from the white dwarf target (orange) than in the light curve extracted at the position of the white dwarf (blue).
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Residual between amplitude heatmap and the best-fit single-star model for two simulated stars with shared frequencies that are in phase with each other. The black “X” marks the fit location, and the gray circles mark the locations of the two stars. Model values are greater than the measured amplitude distribution in the bright yellow pixels, and less than the amplitudes in the dark blue pixels.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Predicted standard errors from the fitting procedure (solid lines) and the observed standard deviation of the fit residuals (points) as a function of S/N in the aperture. The S/N is computed as the signal amplitude divided by mean amplitude in the periodogram of the light curve. We ran 1000 simulations for each S/N value tested.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Same as Figure 8 for shared frequencies that are π out of phase with each other.