adsabs/AstroCLIMB huggingface dataset:
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Example of the setup for shear bias (α) estimation. Top panel: mean tangential shear. Blue points are the mean galaxy shears in a radial bin for 30 realizations of z = 0.059 clusters; error bars are standard errors of the mean. The input NFW tangential shear is plotted as a red line. Middle panel: difference between measured and input tangential shears. Bottom panel: cross shear. The gray-shaded regions indicate the regime where the linearized implementation of Metacalibration is invalid. The SUPERBIT shear calibration analysis will be presented in a forthcoming paper by S. Everett et al.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Left: rendering of SUPERBIT effective (pixel-convolved) PSF in the b filter. Right: Gaussian approximation to b PSF with FWHM = 0.″315. In both panels, intensity values have been normalized so that the total flux in each image sums to unity; the color scale represents relative flux or intensity.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Size–magnitude diagram for objects detected in a single-epoch exposure. Blue points represent all sources; orange points show stars supplied to the PIFF software; dark red star markers show stars selected by the PIFF software for PSF modeling.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Simulated three-hour SUPERBIT observation of a galaxy cluster in the b band using the jitter+optics (“optics-on”) PSF. The central ﹩6^{\prime} \times 3^{\prime} ﹩ region of the simulation is shown. Pixel values represent background-subtracted ADU.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Example of ρ statistics computed from PSF model residuals for a simulated single-epoch exposure. Negative correlations are shown in absolute value and connected to neighboring bins by dotted lines. Isolated points show correlations that changed from positive to negative or vice versa.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Redshift distribution for weak-lensing source galaxies and bootstrapped reference NFW catalog in one simulated observation of a cluster at z = 0.3.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Example MRS mosaicked observations of the bright O9V star 10 Lac (JWST Program ID 1524). The top-left panel shows the flux-calibrated 2D detector-level data for Channels 1A+2A, the top-right panel shows a 5 μm plane of the Ch1A drizzled data cube, and the bottom panel shows the 4.9–27.9 μm spectrum extracted from the drizzled data cube. The 2D detector image and 3D cube image are both in calibrated surface brightness units and are shown here with an identical logarithmic stretch. Values in the data cube that fall outside the IFU footprint or otherwise have no valid data (gray regions in the top-right panel) are set to NaN by default by the JWST pipeline. Faint artifacts surrounding the source are due to imperfections in the cruciform artifact correction (see discussion by P. Patapis et al. 2023b, in preparation).
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Left: general case detector diagram in which the dispersion axis is tilted with respect to the detector columns/rows, and the four corners of a given pixel (bold red outline) each have different wavelengths λ and along-slice coordinates α. Right: projection of this generalized detector pixel into the volumetric space of the final data cube. The red hexahedron represents the detector pixel, where the three dimensions are set by the along-slice, across-slice, and wavelength coordinates. The regular gray hexahedra represent voxels in a single wavelength plane of the data cube. For clarity, the cube voxels are shown aligned with the (R.A., decl.) celestial coordinate frame, but this choice is arbitrary.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: MRS PSF FWHM in the along-slice (blue squares) and across-slice (orange diamonds) directions recovered from drizzled data cubes of point sources observed during commissioning (P. Patapis et al. 2023b, in preparation). The solid black line represents a linear fit to the observed data. The solid red line represents the theoretical diffraction limit for a 6.5 m mirror, while the dashed black line represents Nyquist sampling (defined as two samples per diffraction-limited FWHM). The dashed blue and orange lines represent the sampling provided in the along-slice direction by the detector pixel scale and in the across-slice direction by the IFU slicer width, respectively.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Schematic overview of the MIRI MRS IFU. Left panel: footprint of the IFUs for Channels 1–4 (blue, green, orange, and red regions, respectively) using their A grating setting. Individual slices have been drawn and numbered for Channel 4A. Middle panel: layout of the dispersed spectra on the two Si:As detectors. Channels 1/2 and 3/4 share detectors, and the dispersion direction switches between the two. Slices that are adjacent on the sky are interleaved in the detector plane; numbers illustrate the schematic layout. Right panel: composite data cube reconstructed from the dispersed spectra illustrating the wavelength coverage of each of the 12 MRS spectral bands. Since the IFU field of view (FOV) grows with wavelength, this data cube is in practice akin to a stepped pyramid.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: Our MAP fit to the HST observations. In the upper panels, we show the joint systematics and transit fit to the raw data. In the lower panels, we apply the systematics correction; the resulting light curves contain only residual noise and, in the case of A, the transit. The error bars in the upper panel show photon noise, while in the lower panel we also include our estimated jitter term in quadrature. A y-axis offset has been applied to each light curve for clarity.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: Our mass and radius estimates for LTT 1445Ab and c, including our posterior samples. We overplot composition curves from Zeng et al. (2019), illustrating the mass–radius relation for 100% rock, 100% iron, Earth-like (32.5% Fe+67.5% MgSiO3), and water-world (50% water+50% Earth-like) compositions. Both planets fall along the Earth-like composition curve. For comparison, we also include other small planets around M dwarfs (<0.6 M ⊙) with planetary masses and radii measured to better than 20% error, as tabulated in the NASA Exoplanet Archive (Akeson et al. 2013; accessed 2023 May 22).
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: We compare the TESS response function (blue) to the HST setup used in this work (orange). In red, we overplot the normalized flux for M dwarf models (Allard et al. 2012) for a range of temperatures relevant to the LTT 1445ABC system. For a model 3300 K M dwarf (analogous to LTT 1445A), the effective central wavelength of the two instruments is very similar (dotted vertical lines): roughly 8300 Å for TESS and 8100 Å for HST.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: A corner plot showing our posterior distributions for some key parameters of our LTT 1445Ac fit. In orange, we highlight the 3% of samples consistent with a grazing geometry. The grazing solutions tend toward large impact parameters, transit depths, and stellar radii.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: Our HST aperture photometry prior to removal of systematics. Each star is normalized to its median flux across the two-visit observing campaign. A and B have been shifted by a constant offset such that the light curves do not overlap. The transit occurs at the end of the second orbit.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: The phased light curve of LTT 1445A, highlighting the transit of planet c. The detrended TESS observations are show in black and our new HST observations in orange. In blue, we show our MAP orbital solution.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Top: 54 yr S-index time series for λ Ser. Observations are shown from MWO HKP (red) and Keck HIRES-2 (purple) with seasonal means (black). Bottom: Lomb–Scargle periodogram of the time series, with MWO-only in red, Keck-only in purple, and the composite time series in black. Dashed lines indicate portions of the periodogram beyond the duration of the time series. The top three peaks in the composite time series are indicated with green vertical lines. The periodogram is expressed in units of signal amplitude normalized by a standard deviation. The data behind the top panel of this figure are available in machine-readable format.(The data used to create this figure are available.)
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Large-scale surface magnetic geometry of λ Ser. The three panels display the field components in spherical coordinates, adopting an equatorial projection. Color bars on the right show the field strength in gauss. Vertical ticks above the top panel indicate observed rotational phases. Latitudes below −40° are not observed.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Stokes V polarization profile for λ Ser from LBT observations on 2021 May 24. The mean profile is shown as a black line, with uncertainties indicated by the gray shaded area. The red and blue lines are model profiles assuming dipole geometry and fixed inclination i = 50° with different obliquity angles β.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Stokes V LSD profiles obtained with Neo-NARVAL (black dots) and synthetic profiles produced by ZDI (red curves). Successive observations are vertically shifted for clarity, and the rotational phase Φ of the observation is listed along the right side.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Power spectrum (top) and echelle diagram (bottom) centered on the power excess due to solar-like oscillations detected in λ Ser. Blue solid lines and circles indicate extracted radial (l = 0) modes, while red dashed lines and squares show extracted dipole (l = 1) modes.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Evolution of the wind braking torque with Ro from the calibration of Corsaro et al. (2021). Points are grouped by Gaia color, corresponding to solar analogs (yellow circles) and hotter (blue triangles) or cooler (red squares) stars. The empirical constraint for Rocrit on this scale is shown with a vertical dashed line.
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: The SED of λ Ser. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).
Paper: Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Authors: Travis S. Metcalfe, Derek Buzasi, Daniel Huber, Marc H. Pinsonneault, Jennifer L. van Saders, Thomas R. Ayres, Sarbani Basu, Jeremy J. Drake, Ricky Egeland, Oleg Kochukhov, Pascal Petit, Steven H. Saar, Victor See, Keivan G. Stassun, Yaguang Li, Timothy R. Bedding, Sylvain N. Breton, Adam J. Finley, Rafael A. García, Hans Kjeldsen, Martin B. Nielsen, J. M. Joel Ong, Jakob L. Rørsted, Amalie Stokholm, Mark L. Winther, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Klaus G. Strassmeier, Sandra V. Jeffers, Stephen C. Marsden, Aline A. Vidotto, Sallie Baliunas, Willie Soon
Figure caption: Chandra HRC-I image of λ Ser illustrating the source and innermost of two background regions used for the CR measurement (see Section 2.3 for details).
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Median fiber positioning error over the focal plane before (blue) and after (red) implementing the turbulence correction code. The floor at about 3  μm is likely set by the intrinsic rms centroiding error of a spot image as measured by spotmatch using the FVC CCD.
Paper: Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane
Authors: S. Kent, E. Neilsen, K. Honscheid, D. Rabinowitz, E. F. Schlafly, J. Guy, D. Schlegel, J. García-Bellido, T. S. Li, E. Sanchez, J. Silber, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, P. Doel, D. J. Eisenstein, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A. Gontcho, J. Jimenez, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, J. Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, M. Rezaie, A. J. Ross, G. Rossi, M. Schubnell, H. Seo, Gregory Tarlé, B. A. Weaver, R. Zhou, Z. Zhou, H. Zou
Figure caption: Amplitude of the two nonaxisymmetric modes in Figure 4 in the distortion model for a set of 210 exposures taken at various ADC settings. The quantity plotted is the residual between the measured coefficient and that predicted by the telescope optical model. Left: E mode. Right: B mode. Turbulence affects the amplitude of the former (rms scatter of 2.4 μm) but not the latter (rms scatter of 0.3 μm).