adsabs/AstroCLIMB huggingface dataset:
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper left: measured period ratios between P  B  and P  A  for the 97 quadruple candidates from TESS that pass vetting tests, compared with select integer ratios. Upper right: distribution of the number of systems with periods ratio P  A /P  B  smaller than 4 (72 out of 97 systems). Lower left: same as upper left but for a simulated set of systems. Lower right: number of simulated systems with period ratios that match to within 4% one of the rational numbers 1:1, 5:4, 4:3, 3:2, 5:3, 2:1, 5:2, or 3:1. See text and Table 3 for details.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panel: FFI lightcurve of quadruple candidate TIC 52856877. The system consists of two EBs with P  A   = 5.1868 and P  B   = 18.5864 days, highlighted in the figure. Lower panels: measured eclipse-time variations for P  A  (left panel) and P  B  (right panel), indicating dynamical interactions between the two binaries and suggesting that the system is gravitationally bound.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Left panel: R.A. and decl. of the quadruple candidates in this catalog. Middle panel: the respective astrometric_excess_noise (AEN) and astrometric_excess_noise_sig (AENS) as measured by Gaia. We note that both are on a logarithmic scale. Right panel: corresponding distribution of the renormalized unit weight error (RUWE) as a function of the AEN. The dashed horizontal line indicates RUWE = 1.5, the value above which the astrometry is likely affected by a presumptive wide companion.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panels: measured ﹩e\,\cos (\omega )﹩ (left panel) and ﹩e\,\sin (\omega )﹩ (right panel) for the corresponding binary A (blue) and B (red) for each quadruple candidate exhibiting both primary and secondary eclipses. Most ﹩e\,\cos (\omega )﹩ and ﹩e\,\sin (\omega )﹩ ratios cluster around zero. Lower left panel: corresponding eccentricity and omega values with the associated measured uncertainties, calculated by propagating the uncertainties in ﹩e\,\cos (\omega )﹩ and ﹩e\,\sin (\omega )﹩ into those for e and ω. Lower right panel: eclipse depth ratios, showing no clear preference.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Same as Figure 15 but for quadruple candidate TIC 45160946. The system consists of two EBs with P  A   = 3.5163 and P  B   = 7.8462 days, highlighted in the figure. Lower panels: measured eclipse-time variations for P  A  (left panel) and P  B  (right panel), indicating dynamical interactions between the two binaries and suggesting that the system is gravitationally bound.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panel: long-cadence TESS eleanor lightcurve of PTIC 316464966 showing two sets of eclipses, with periods of P1 = 1.06 days and P2 = 0.24 days. The TIC lists two stars separated by about 1.″11, TIC 1821336783 and TIC 1821336772, with respective magnitudes of T = 13.83 mag and T = 14.27 mag. Either star can produce either set of eclipses, and the separation between them is too small for reliable photocenter measurements. This is an example of a potential false positive due to blended stars that are too far apart to be of interest for this study (in this case ∼1000 au).
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Same as the second and third panels in Figure 10 but for a primary eclipse of binary B of TIC 285681367 (see Figure 2). Here the generalized Gaussian and hyperbolic secant functions are clearly the better representation of the eclipse compared with a Gaussian. The flatter/sharper the eclipse bottom is, the better the former two fit the data.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Mapping between Kerr–Schild (KS) coordinates and funky modified Kerr–Schild (FMKS) coordinates. Left: lines of constant FMKS radial coordinate x 1 (vertical) and latitudinal coordinate x 2 (left-to-right) plotted vs. KS radius r and elevation θ. Right: same as left but plotted in a Cartesian embedding with ﹩x=r\sin \theta ﹩ and ﹩z=r\cos \theta ﹩. FMKS coordinates concentrate resolution near the midplane θ = π/2 and away from the poles θ = 0, π at small radii.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panel: long-cadence TESS eleanor lightcurve of TIC 285681367, showing two sets of eclipses with period P  A   = 2.37 days and P  B   = 3.97 days. Second and third panels from top: phase-folded lightcurve for binary A and binary B, respectively. For clarity, the lightcurve was disentangled such that the eclipses of the other binary were removed (Powell et al. 2021). Lower left and middle panels: TESS difference images (13 × 13 pixels) for P  A  and PB , respectively, showing the pixels changing during the corresponding primary eclipses. The axes represent the corresponding relative pixel number along the x-axis (pixel column number) and y-axis (pixel row number). The small red symbols represent the measured photocenter for the individual primary eclipses of each respective binary, and the large red circle shows the corresponding average photocenters. The black star is the catalog position of the target, and the dashed contour represents eleanor’s aperture used to extract the target’s FFI lightcurve. Lower right panel: Skyview image (also 13 × 13 pixels) of the target’s TESS aperture showing known nearby sources down to G = 21 mag. The photocenter analysis shows that both sets of eclipses are on target.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: An example of a nominal false positive (TIC 458740798) caused by a genuine quadruple candidate (TIC 458740670) in the field. First row: long-cadence TESS eleanor lightcurve of TIC 458740798 for sector 36 (the false positive). Second row: same as first row but for TIC 458740670 (the quadruple). Note how all eclipses are deeper on TIC 458740670, already indicating that it is the source of the eclipses. Third row, left and middle panels: photocenter analysis for TIC 458740798, showing the difference images (left for binary A with P = 6.26 days, middle for binary B with P = 7.02 days), along with the pixel-response function–based measurements of the individual photocenters (small red dots) and average photocenter (large open circle). The black star symbol indicates the catalog position of TIC 458740798. The measured photocenters are centered on a location about 3 pixels above TIC 458740798—near the position of TIC 458740670. Third row, right panel: Skyview image of the TESS aperture for TIC 458740798 (at the center of the image, marked with a black plus symbol), highlighting the true source of the eclipses TIC 458740670 (red arrow). Fourth row: same as third row but for TIC 458740670—a genuine quadruple candidate—showing that the measured photocenters coincide with the location of TIC 458740670. Note that eleanor’s aperture for TIC 458740670 is adjacent to the target, and as a result the true eclipse depths are larger than those seen in the lightcurve (second row).
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Long-cadence TESS eleanor lightcurve (upper panel) and photocenter analysis (lower left and middle panels) of TIC 59769582. The analysis shows that binary A with P  A   = 1.57 days is on target (lower left panel), while binary B with P  B   = 13.5 days is off target (lower middle panel), about 2 pixels SW of TIC 59769582. The lower right panel shows the Skyview image of the TESS aperture for TIC 59769582 (at the center of the image, marked with a plus symbol), highlighting the source of the P  B  eclipses (red arrow). This is an example of on-target EB + field star EB false positive.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Example quadruple false positive for scenario (1) described in Section 3.1. First row, left panel: sector 14 QLP lightcurve of TIC 354575570 as used by the visual surveyors for the detection of two apparent sets of eclipses. First row, right panel: 15 × 15 pixels Skyview image of the target’s TESS aperture showing known nearby sources. Middle and lower rows: Lighkurve visualization of the selected pixels (white contours in right panels) and the corresponding lightcurve (left panels). The target is a quadruple false positive as one of the EBs is clearly off target.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: First and second row: long-cadence TESS eleanor lightcurve of TIC 53201931, a triply eclipsing triple star producing a pair of tertiary elipses in sector 9 (first row, 30 minutes cadence) and in sector 34 (second row, 10 minutes cadence). Third row, left and right panels: photocenter measurements for the inner binary (left, with a period of 8.9 days) and for the third star (right, with a period that is ∼700/N, where N is an integer). Note how the pair of tertiary eclipses change shape and order—the “smoking gun” signature of a third star orbiting the EB. This is an example of on-target false-positive quadruple due to a triple star.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Illustrative example of a screenshot of LcTools used to detect and analyze the quadruple candidate TIC 285681367. The upper panels show the detrended TESS QLP lightcurve of the target, along with the detrending options. The lower panels show the phase-folding setup, options, and results, as well as a zoomed-in section of the lightcurve centered on a particular eclipse used to fix the ephemeris.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Same as Figure 3 but for false-positive scenario (2). First row, left panel: TESS-CPM lightcurve for TIC 415189369 (Hattori et al. 2020). The target is a quadruple false positive as the relative depths of the two sets of eclipses scale differently depending on the selected pixel. Middle and lower rows: Lighkurve visualization of the selected pixels (white contours in right panels) and the corresponding lightcurve (left panels).
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Same as Figure 5 but for TIC 262535168. The two EBs seen in the lightcurve originate from two different targets, neither of which is TIC 262535168, as highlighted on the Skyview image. This is an example of a false positive due to field EB (star 1) + field EB (star 2).
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: GRMHD simulation of a MAD accretion flow with a * = 0.5. This simulation was initialized with an r in = 20, ﹩{r}_{\max }=41﹩ torus and run at a resolution of 448 × 224 × 224 zones in the r, θ, and ϕ directions, respectively. Top panels show rest-frame plasma density in arbitrary units at three different times over the course of the simulation; the line integral convolution technique is used to represent the motion of the plasma. The bottom panels show magnetization at the same times as the top panels with overplotted contours of the axisymmetrized vector potential component A  ϕ , which give a sense of field strength and disorder. The black hole event horizon is plotted as a dark circle. As the simulation evolves, the flow becomes increasingly turbulent and a high-magnetization jet region opens around the poles.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Image of the supermassive black hole at the center of the Messier 87 galaxy at 230 GHz produced by the Event Horizon Telescope Collaboration from observations taken on 2017 April 11. Left: total intensity of light shown in units of brightness temperature T  b  = S λ 2/2kΩ, where S is the (total) flux density, λ is the observing wavelength, k is the Boltzmann constant, and Ω is the solid angle of the observing element. Right: linear polarimetric data from the same observation plotted atop gray-scale total intensity as in the left panel. The orientation of each tick corresponds to the electric-vector position angle projected onto the image plane, and its color encodes the local fractional linear polarization. Tick marks are only shown in regions where the local total intensity is >1/10 its maximum value and fractional linear polarization is >1/5 its maximum. The FWHM of the largest Gaussian blurring kernel used in image reconstruction is represented as a circle with diameter 20 μas in the bottom right of the panel. See EHTC IV and EHTC VII for more details.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Decomposition of the total intensity into the first three subrings for a snapshot from the high spin a * = 0.94 MAD model with r low = 1, r high = 10, and i = 17°. The intensities in the n = 0, n = 1, and n = 2 subrings are reported in the right three panels, and the location of the critical curve is plotted as a dashed line in green. The total flux density, whose decrease is governed by angle-dependent Lyapunov exponents in the limit of large n for optically thin systems, is given in the top right of each panel. The left panel shows a composite image produced by adding the n = 0 subring in red, n = 1 subring in blue, and n = 2 subring in green. The visual appearance of each subring image is due to the details of the underlying emission, although the geometric extent of each image is due to the spacetime.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Comparison of density, plasma β, and magnetization σ in the midplane of MAD and SANE simulations in steady state. Both simulations were run with an intermediate spin a * = 0.5. In the MAD simulation, the accretion proceeds in thin strands, contrasting the steady but turbulent disk-like SANE accretion mode. The evacuated regions in the MAD simulation with low β and high σ are magnetic bubbles produced during the flux ejection events that episodically recur when an excess of magnetic flux has been trapped on the event horizon.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Time series of flux variables from the MAD a * = 0.5 simulation. Top panel: mass accretion rate in arbitrary code units vs. time. Center panel: dimensionless magnetic flux ϕ vs. time. Bottom panel: light curves at ν = 230  GHz for r low = 1 and different r high values. The light curves have been scaled to match a 1 Jy target flux density over the last 5000 GM/c 3 of the simulation. The first half of the simulation is dominated by a transient from the torus initial condition. Notice that stability in ﹩\dot{m}﹩ and ϕ does not necessarily equate to stability in the 1.3 mm light curve.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Example polarimetric images of MAD a * = 0.5 simulation produced by ipole with (bottom) and without (top) blurring to 15 μ as Gaussian beam. Panels show total intensity, linear polarization fraction, electric-vector position angle (EVPA), and circular polarization fraction. The brightness of each pixel has been scaled to the total intensity; the patterns in linear polarization, EVPA, and circular polarization continue into the dark regions. Blurring decreases the observed linear polarization fraction in regions where EVPA is rapidly varying.
Paper: PATOKA: Simulating Electromagnetic Observables of Black Hole Accretion
Authors: George N. Wong, Ben S. Prather, Vedant Dhruv, Benjamin R. Ryan, Monika Mościbrodzka, Chi-kwan Chan, Abhishek V. Joshi, Ricardo Yarza, Angelo Ricarte, Hotaka Shiokawa, Joshua C. Dolence, Scott C. Noble, Jonathan C. McKinney, Charles F. Gammie
Figure caption: Photograph of an oil field near Patoka in Marion County, Illinois published in 1940 February. The PATOKA pipeline is named for the Patoka Oil Terminal in Patoka, Illinois, which connects several oil pipelines in the second Petroleum Administration for Defense District. Photo credit: Arthur Rothstein/Farm Security Administration, LC-DIG-fsa-8a13148.