adsabs/AstroCLIMB huggingface dataset:
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: Error adjustment factor for the centroid, i.e., ﹩{p}_{{\mu }_{x}}﹩, on the left and sigmas, i.e., ﹩{p}_{{\sigma }_{{xx}}^{2}}﹩, on the right. The two are basically identical but are shown separately for the sake of clarity. The red curve is the piecewise linear interpolation. The approximate logistic function is shown in Equations (37) and (38).
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: The correction factor f ∞ when convergence is allowed is shown on the left. The correction factor g ∞ when convergence is allowed is shown on the right. Clearly, both factors blow up at low S/Ns, implying that convergence is only feasible at a fairly high S/N.
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: This plot shows the performance of the traditional moment matching algorithm in blue, forced measurement without truncation in red, and forced measurement with truncation and bias correction in black. Individual frame measurements were performed in the 146 i-band and 151 r-band images for all sources inside the black box shown in Figure 14. The x-axis is divided into nine equal bins in log space. The points and the error bars shown are the median and standard deviation after sigma clipping in each bin. It is clear that our method of forced measurement with bias and truncation correction outperforms in every aspect. The red and black data points have been shifted slightly on the x-axis for visual clarity.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The FFI light curve and folded light curve for TIC ID 149989733 sector 10. This light curve was chosen as a typical example of the light curves identified by our NN. A notable aspect is that only two or three data points exist for each period (1.326 hr), resulting in the periodicity not being clear to a human observer in the unfolded light curve. Despite no specific periodicity-detecting mechanisms being included in the NN, it learns to identify such periods in the unfolded data. The time is given in TESS Barycentric Julian Day (BTJD) time (Tenenbaum & Jenkins 2018). With the Julian Day in the Barycentric Dynamical Time standard (BJD), BTJD = BJD −2,457,000.0. BJD is used for its accurate time standard, which accounts for many different timing corrections, including leap seconds (e.g., Eastman et al. 2010). The flux given is median-normalized flux for the light curve. Color is based on unfolded time. This is an example from our δ Sct clusters (see Section 4.3 for clusters' explanation).
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The absolute V magnitude vs. the period of the short-period variables. Note that these are the absolute V magnitudes provided by the TIC, which does not assume that the targets are binaries. Partition colors and partition lines are chosen based on a partitioning in log luminosity vs. log period relations described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: An overview of the architecture of the CNN used in this work. See Olmschenk et al. (2021) for details. All convolution/dense layers within a block use a number of filters/units equivalent to the size of the last dimension of their output tensor. A kernel size of 3 is used in all convolutional layers. For clarity of the diagram, three deviations from the diagram blocks are not shown. First, the first convolution block and the last dense block do not apply dropout or batch normalization. Second, the final convolution block uses a standard dropout instead of spatial dropout, as the following layer is a dense layer. Third, pooling is only used by the first six convolution blocks. The remaining convolution blocks do not use pooling.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The FFI light curve and folded light curve for TIC ID 159971257 sector 23. This is an example from our MS binary cluster with clearly distinct binary signal peaks (see Section 4.3 for clusters' explanation). Presented the same as Figure 1. See Figure 1 for details.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The period distribution of the short-period variables as estimated by our pipeline. Note that for binary systems this estimated period may be half of the system’s full orbital period.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: A kernel density estimation of effective temperature vs. period of the short-period variables. The effective temperature of the targets is taken from the TIC.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: A random set of examples of synthetic periodic signals to be injected into TESS light curves as training data. Two periods of each synthetic signal are shown.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The radius vs. the period of the short-period variables colored by the variable effective temperature. Due to high effective temperature outliers, the upper limit of the effective temperature scale is restricted to 11,000 K, and any targets above this effective temperature are shown as red squares. Note caveats given in Section 4.3 about how these values are estimated and how the estimate value may differ from the true value, especially with regard to binaries.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The relative amplitude vs. the period of the short-period variables colored by the variable effective temperature. Due to high effective temperature outliers, the upper limit of the effective temperature scale is restricted to 11,000 K, and any targets above this effective temperature are shown as red squares.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The powers of the fundamental mode and first-overtone mode. Data points are colored by the partitions described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The mass vs. the period of the short-period variables. Due to high effective temperature outliers, the upper limit of the effective temperature scale is restricted to 11,000 K, and any targets above this effective temperature are shown as red squares.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: A kernel density estimation of the TESS magnitudes of the short-period variables. Magnitude values come from the TIC. Distributions are colored by the partitions described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: A kernel density estimation of the parallaxes of the short-period variables. Parallax values come from the TIC. Distributions are colored by the partitions described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: A kernel density estimation of the colors of the short-period variables. Color values come from the TIC. Distributions are colored by the partitions described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The effective temperature vs. luminosity of the short-period variables. Distributions are colored by the partitions described in Section 4.3.
Paper: Short-period Variables in TESS Full-frame Image Light Curves Identified via Convolutional Neural Networks
Authors: Greg Olmschenk, Richard K. Barry, Stela Ishitani Silva, Jeremy D. Schnittman, Agnieszka M. Cieplak, Brian P. Powell, Ethan Kruse, Thomas Barclay, Siddhant Solanki, Bianca Ortega, John Baker, Mamani Yesenia Helem Salinas
Figure caption: The radius vs. the period of the short-period variables. Data points are colored by the partitions described in Section 4.3.
Paper: Keck and Hubble Observations Show that MOA-2008-BLG-379Lb is a Super-Jupiter Orbiting an M Dwarf
Authors: David P. Bennett, Aparna Bhattacharya, Jean-Philippe Beaulieu, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Clément Ranc, Natalia Rektsini, Sean K. Terry, Aikaterini Vandorou, Jessica R. Lu, Jean Baptiste Marquette, Greg Olmschenk, Daisuke Suzuki
Figure caption: (a) A 32″ × 32″ section of the coadded sum of 12 × 60 s exposures with the Keck NIRC2 narrow camera images taken 10 years after the microlensing event, with the target location indicated by a blue square. The images in panels (b) and (c) are 2.5″ × 2.6″ close-ups of the target with the Keck K  s  band and the Hubble WFC3/UVIS F814W passband, respectively. The green and red dots are the best-fit positions of the lens and source stars. The coadded Hubble frame, taken in 2013, involves no image resampling. Instead, each pixel of the individual Hubble images is divided into 100 × 100 subpixels, which are each assigned the same flux value. Thus, image (c) shows full-size pixels with the observed dither offsets accurate to 0.01  pixels.
Paper: Keck and Hubble Observations Show that MOA-2008-BLG-379Lb is a Super-Jupiter Orbiting an M Dwarf
Authors: David P. Bennett, Aparna Bhattacharya, Jean-Philippe Beaulieu, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Clément Ranc, Natalia Rektsini, Sean K. Terry, Aikaterini Vandorou, Jessica R. Lu, Jean Baptiste Marquette, Greg Olmschenk, Daisuke Suzuki
Figure caption: The color–magnitude diagram of OGLE III stars within 90 arcsec of microlensing event MOA-2008-BLG-379 (black dots), with the Hubble color–magnitude diagram of Baade’s window (green dots; Holtzman et al. 1998), transformed to the same extinction and Galactic bar distance as the MOA-2008-BLG-379 field. The red spot is the red clump giant centroid; the source and lens magnitudes from our Hubble observations are indicated in blue and orange. As Table 2 indicates, the V-band (F555W) Hubble images detect the lens star (star 1) at ∼1.2σ significance, so the Hubble measurements can be considered only an upper limit on the V-band brightness of the lens (and planetary host) star. The magenta spot indicates the lens star color and magnitude inferred from our Markov Chain Monte Carlo calculations using the constrained eesunhong light-curve modeling code. Since the lens star is likely to be in the disk or the near side of the bulge, it is typically brighter than the bulge main sequence.
Paper: Keck and Hubble Observations Show that MOA-2008-BLG-379Lb is a Super-Jupiter Orbiting an M Dwarf
Authors: David P. Bennett, Aparna Bhattacharya, Jean-Philippe Beaulieu, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Clément Ranc, Natalia Rektsini, Sean K. Terry, Aikaterini Vandorou, Jessica R. Lu, Jean Baptiste Marquette, Greg Olmschenk, Daisuke Suzuki
Figure caption: The Bayesian posterior probability distributions for the planetary companion mass, host mass, their separation, and the distance to the lens system are shown with only light-curve constraints in blue and with the additional constraints from our Keck and Hubble follow-up observations in red. The central 68.3% of the distributions are shaded in darker colors (dark red and dark blue), and the remaining central 95.4% of the distributions are shaded in lighter colors. The vertical black line marks the median of the probability distribution of the respective parameters.
Paper: Keck and Hubble Observations Show that MOA-2008-BLG-379Lb is a Super-Jupiter Orbiting an M Dwarf
Authors: David P. Bennett, Aparna Bhattacharya, Jean-Philippe Beaulieu, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Clément Ranc, Natalia Rektsini, Sean K. Terry, Aikaterini Vandorou, Jessica R. Lu, Jean Baptiste Marquette, Greg Olmschenk, Daisuke Suzuki
Figure caption: The best-fit light curve with the constraints from the high angular resolution follow-up data, as explained in Section 4.3. This is the model from the third column of Table 3, with u 0 > 0 and s > 1.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: M–R distribution (colored by the planet’s equilibrium temperature and sized by the orbital eccentricity) for confirmed exoplanets presented in the Encyclopædia of Exoplanetary Systems (https://exoplanet.eu/home/) as of 2024 March. The red star represents TOI-1173 A b, and the dashed black line is the theoretical M–R curve for a planet composed of cold Hydrogen according to the H-REOS.3 equation of state from Becker et al. (2014), to which TOI-1173 A b's composition seems to be alike. Constant-density curves are shown with the dotted–dashed lines, and the blue one represents the density threshold adopted in this work for puffy planets. In terms of period, semimajor axis, and mass, TOI-1173 A b is similar to TOI-1420 b and WASP-107 b. The black open circles represent the planets from the wide binary sample with densities higher than 0.3 g cm−3, while the black crosses represent planets on S-type orbits (planets that orbit just one star in a binary pair) with masses between 5 and 35 M ⊕.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Left: companion sensitivity for the near-infrared AO imaging. The black points represent the 5σ limits and are separated in steps of 1 FWHM. The purple represents the azimuthal dispersion (1σ) of the contrast determinations (see the text). The inset image is of the primary target showing no additional close-in companions. Right: SAI 2.5 m I  c -band speckle sensitivity curve for TOI-173 A. The speckle image also does not show evidence of close companions.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Target pixel file of TOI-1173 A (white cross) from the TESS observations in Sector 48. The SPOC pipeline aperture is overplotted with shaded red squares, clearly showing that there is no contamination by the companion star TOI-1173 B (marked with the number 2). The projected separation between the components (numbers 1 and 2) is ∼86″.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Radial velocity and the relationship with TOI-1173 A’s activity indicators dLW, CrX, and Hα, plus the Na doublet for the Blue channel and the Ca II infrared triplet for the Red channel of MAROON-X spectra. The colors indicate the phase at P LS = 7.076 days. The Pearson r correlation index and the associated p-values are indicated at the top of each panel.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Upper panel: BLS periodogram for TOI-1173 A b's observations. The prominent period of P = 7.066 days is indicated as a red strip, along with lower (P/n, n = 1, 2, 3, 4) and upper (P × n) harmonics, in gray. Bottom panels: detrended TESS 2 minute cadence PDC light curves. Transit events are visible every 7.066 days.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Phase-folded TESS light curve (upper panel) and MAROON-X plus HIRES radial velocities (bottom panel) joint models of TOI-1173A b. The red curves show 20 samples drawn from the posterior. The associated residuals are shown below each panel.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Envelope mass fraction estimates with tides (f env, t) and without tides (f env, 0) of TOI-1173 A b. The horizontal dashed lines represent the lower limit of the reduced tidal quality factor (﹩{\mathrm{log}}_{10}Q^{\prime} ﹩). The mean and standard deviation of f env, 0 are represented by the vertical gray bar. The colored regions indicate the 2σ contours of the posterior distributions of ﹩{\mathrm{log}}_{10}Q^{\prime} ﹩ and f env, t after accounting for tides.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Planet density as a function of stellar insolation. TOI-1173 A b is indicated in red. The circles represent the planets with host stars sharing similar physical parameters as TOI-1173 A, colored by their equilibrium temperatures and sized by the planet’s semimajor axis.
Paper: TOI-1173 A b: The First Inflated Super-Neptune in a Wide Binary System
Authors: Jhon Yana Galarza, Thiago Ferreira, Diego Lorenzo-Oliveira, Joshua D. Simon, Henrique Reggiani, Anthony L. Piro, R. Paul Butler, Yuri Netto, Adriana Valio, David R. Ciardi, Boris Safonov
Figure caption: Planetary density as a function of the planetary mass of exoplanets obtained from the Encyclopædia of Exoplanetary Systems as of 2024 March. The characteristic “V” shape, and the size of the points, which scale with the planetary radius, denote two regimes of planets. The circles are colored according to their equilibrium temperature. TOI-1173 A b (green star) and the other puffy super-Neptunes (open blue squares) lie in the transition region.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: (A) Overlaid histograms of stellar radii of single-transiting-planet host stars (blue) and compact multiple system host stars (pink). (B) Overlaid histograms of stellar mass of single-transiting-planet host stars (blue) and compact multiple system host stars (pink). (C) Overlaid histograms of stellar age of single-transiting-planet host stars (blue) and compact multiple system host stars (pink). The uncertainty on the stellar ages used are immense. (D) Stellar age vs. stellar mass for host stars of single-transiting planetary (blue) and compact multiple systems (pink). Most of our stellar sample host stars have stellar radius values between 0.5 R ☉ and 0.7 R ☉ and stellar mass values between 0.5 M ☉ and 0.7 M ☉ with a tail toward smaller masses and radii. The single-transiting planetary systems and the compact multiples do not have significantly different stellar parameters, and derived differences in the planetary samples are unlikely to be a consequence of their host star population.