adsabs/AstroCLIMB huggingface dataset:
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Correlation between the precision of estimated [Ba/Fe] and the S/N of spectra. The red circles and the error bars represent the averages and standard errors of the bins, respectively.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Examples of LAMOST MRS spectra marked by gray circles and synthetic spectra with a range of Ba abundances are shown with different colors and line styles (provided in the legend); the best-matching spectra are shown in red solid lines.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Distributions of [Ba/Fe], as a function of [Fe/H], for LAMOST MRS DR9 using stellar parameters from the LR LASP, shown as a 2D histogram, color coded by number density.
Paper: Barium Abundances from the LAMOST Medium-Resolution Survey Stellar Spectra
Authors: Tian-Yi Chen, Jian-Rong Shi, Hong-Liang Yan, Timothy C. Beers, Chun-Qian Li, Ming-Yi Ding, Xiao-Jin Xie, Liu Shuai, Zeming Zhou, Yao-Jia Tang
Figure caption: Distributions of the stellar parameters for our LAMOST MR sample are shown as gray 2D histograms, with the common stars with available high-resolution spectra indicated by red crosses.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: Accuracy test with homogeneous {B(r), ne(r), N0(r)} fields with callable field generators. The left panel shows the synchrotron {I, Q, U} maps generated by synax, the middle panel shows the residual between synax and the theoretical value, and the right panel shows the relative error between synax and the theoretical value. Unless mentioned otherwise, all healpix maps in this work are in units of kelvin.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: An illustration of the integration points along several sight lines with the number of integration points Nint = 16 in a box of length (40, 40, 10) kpc along the x, y, z directions, respectively. The legend shows the index of the sight line for an NSIDE = 64 healpix map, while the large red dot represents the observer on Earth.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: Upper: standard deviation of the residuals for the simulated maps with different Nint, defined with respect to the map generated with Nint = 2048. Lower: standard deviation of the residuals of a grid B model map compared to an analytical B model map, as a function of grid size Nx. Solid, dotted, and dashed lines represent {I, Q, U} maps, respectively.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: From left to right: simulated synchrotron Q map, mock observation, and optimized synchrotron Q map in units of kelvin with WMAP B, N0 models, and YMW16 ne model at 2.4 GHz. The map has NSIDE = 64 and Nint = 512.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: Reproduced Haslam map by optimizing the B field on grids in units of kelvin. Top left: Haslam map spatially averaged to NSIDE = 64. Top middle: synchrotron I map generated with optimized B field. Top right: residual map of the optimized I map compared with the Haslam map. Bottom left: histogram of residuals. Bottom right: a slice of optimized B magnitude at z = 0 kpc.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: Posteriors for WMAP B field parameters obtained with NUTS. The shaded areas are the 1σ (dark blue) and 2σ (light blue) credible regions, and gray dashed lines indicate the true parameter values. The mock observation map consists of a simulated noiseless map and white noise with standard deviation of 1 mK.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: The blue solid line indicates wall clock time for a single realization with respect to the total number of integration points Ntotal, using a Tesla A100 GPU. The gray dotted line corresponds to the theoretical scaling where time is proportional to Ntotal.
Paper: synax: A Differentiable and GPU-accelerated Synchrotron Simulation Package
Authors: Kangning Diao, Zack Li, Richard D. P. Grumitt, Yi Mao
Figure caption: Left: a slice of the true B field magnitude at z = 0 kpc. Right: a slice of the optimized B field magnitude at z = 0 kpc.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Number of detections versus the mean magnitude of each lightcurve labeled in ZTF OIDs. The top and right panels show the normalized probability density distribution (total area under the curve sums to 1) of x- and y-axis quantities respectively. Objects with lower magnitude have a higher numbers of observations simply because brighter sources are more easily detected. However, there are two separate lines of such a trend because one real source usually has multiple (two in most cases) ZTF OIDs.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: The periodic variable source found by X. Chen et al. (2020) in IC 10. The top panel shows the lightcurve with error bars showing error in magnitude. Different markers represent different ZTF-labeled OIDs under the same source ID. The bottom panels are the folded lightcurves of the two OIDs, fitted with a sine function, and color coded by MJD. This source is identified as a periodic variable in the r band by our algorithm, but did not pass the survival function test in the g band due the relatively large error in g-band magnitude measurements.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Distribution of Sk(χ2) for all lightcurves in the ZTF r and g bands. Lightcurves left of the red dotted line have a 99% or more chance to be variable and are classified as variable. Hatched regions (right of the red dotted line) are excluded.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Distribution of CT for low-FAP, high-QP lightcurves in the ZTF r and g bands. We cut (hatched region) lightcurves left of the red dotted line, and lightcurves in between blue dotted lines, with the exception of extremely low FAP.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Distribution of QP for low-FAP lightcurves in the ZTF r and g bands. We keep lightcurves right of the red dotted line and remove the ones on the left. Hatched regions (right of the red dotted line) are excluded.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Distribution of FAP for variables in the ZTF r and g bands. We keep lightcurves left of the red dotted line as low-FAP lightcurves. Hatched regions (right of the red dotted line) are excluded.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Visualization of our methodology.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: The color–magnitude diagram. The horizontal axis is the mean g − r color, and the vertical axis is the mean r magnitude. Gray lines denotes 1σ in color and magnitude. The top and right panels show the normalized probability distribution of x- and y-axis quantities, respectively. Only sources detected in both r and g bands are included in this plot.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: H-R diagram for IC 10 sources as defined in Section 4.5. The marker shape shows the variability, the color code denotes SIMBAD identification, and the red crosses indicate Chandra detection. There is a nonvariable source with Mr ∼ −13 not drawn in the plot for a better view.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: The mean and standard deviation of magnitudes for UPSILoN periodic sources, with shapes indicating the classification in this work. The dashed line shows the typical observation error in magnitudes at certain magnitude. The error in magnitudes is larger for dimmer (larger 〈m〉 sources). UPSILoN periodic sources identified as nonvariable in this work typically have lower variation (low 〈σm〉) in magnitude compared to variable sources at the similar 〈m〉, and are closer to the dashed line of error in magnitude measurements, showing that our sample of variable sources is prioritizing purity instead of completeness.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Location of ZTF sources overlaid with a Digital Sky Survey color image of IC 10. The contours show the source density relative to the mean density of four background fields. The numbers on the contours show how many sigmas (standard deviation of four background densities) they are away from mean background density. Sources that are within the 25σ density contour, and are not Gaia foreground sources, are defined to be “IC 10 sources.”
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: An example source that is identified as periodic in the r band by our catalog but not by UPSILoN. The top panel shows the lightcurve with error bars showing error in magnitude. Different markers represent two ZTF-labeled OIDs under the same source ID. The bottom panels are the folded lightcurve of the two OIDs, fitted with a sine function, and color coded by MJD. The FAP of the r-band periodicity is 7.29 × 10−64, and the χ2 of the r-band sinusoidal fit is 2.36.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: The distribution of foreground sources (Plxflag=1), distant sources (Plxflag=0), and non-Gaia sources on a color–magnitude diagram. The top and right panels show the normalized distribution of x- and y-axis quantities respectively. Foreground sources are generally brighter and redder (higher g − r color).
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Sources labeled by SIMBAD on the color–magnitude diagram. Blue dots are all the sources included in this catalog, colored dots are SIMBAD matches of different object types, and gray lines denote 1σ in color and magnitude. XMM-Newton and Chandra counterparts are labeled as crosses (×) and pluses (+).
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Physical location of r-band foreground sources (left) and distant (right) sources, overlaid with a Digital Sky Survey color image of IC 10. Foreground sources are more uniformly distributed than distant sources.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Source 128. Different markers represent different ZTF-labeled OIDs.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Sources 242, 557, and 1259, three superred sources that are detected in both r and g bands. These sources are periodic in the r band with periods of 1608, 514, and 595 days respectively. Different markers represent different ZTF-labeled OIDs under the same source ID.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: H-R diagram for foreground sources. The marker shape shows the variability, the color code denotes SIMBAD identification, and the red symbols indicate X-ray emission as detected by Chandra (“X”) or XMM (“+”).
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: First row: Three superred nonperiodic variable sources that are detected only in the r band and have Gaia matches. The average absolute magnitudes of these sources (Sources 490, 1891, and 2307) are 7.58, 4.26, and 10.20 mag. Second row: three superred nonperiodic variable sources detected only in the r band but that do not have Gaia matches. Third row: Two superred nonvariable sources detected only in the r band and that have Gaia matches. The average absolute magnitudes of these sources (Sources 169 and 1695) are 7.07 and 7.55 mag. Different markers represent different ZTF-labeled OIDs under the same source ID.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Folded lightcurves of periodic supergiants with a sinusoidal fit for bands with statistically significant periodicity. The lightcurves are folded by the Lomb–Scargle period if periodic, or by the Lomb–Scargle period of the other band if nonperiodic. The color denotes the MJD of the observation.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Cumulative distribution of time between the closest r- and g-band observations for flaring supergiants in IC 10.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: g − r color with g-band magnitude for source 90 observed after MJD 58750, fitted by a quadratic polynomial. The lower panel shows the Δχ2 of the fit.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Magnitude and color (g − r) of Source 90, with the red vertical line indicating MJD 58750. Different markers represent different ZTF-labeled OIDs.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Source 1108, a typical flaring supergiant. Different markers represent different ZTF-labeled OIDs. The survival function Sk(χ2) of a constant-line model is 8.71 × 10−14 for the r-band lightcurve, and 9.07 × 10−8 for the g-band lightcurve.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: The lightcurve of Source 193 for the fit parameters presented in Table 10.
Paper: ZTF IC 10 Variable Catalog
Authors: Zehao Jin, Joseph D. Gelfand
Figure caption: Lightcurves of selected compact objects. Left: Source 145, a possible white dwarf. This source is identified as a periodic variable in the r band with a periodicity of 746.2 days and a nonperiodic variable in the g band. This source is labeled as an emission-line star in SIMBAD. Right: Source 2008, a possible X-ray binary. This source is identified as a periodic variable in the r band with a periodicity of 21.6 days and a nonperiodic variable in the g band. This source is detected by Chandra. Different markers represent different ZTF-labeled OIDs under the same source ID.
Paper: Absolute Rate Coefficients for Dielectronic Recombination of Sodium-like Iron Ions: Experiment and Theory
Authors: H. K. Huang, W. Q. Wen, Z. K. Huang, Y. Yuan, C. Y. Zhang, R. Si, S. J. Wu, C. Y. Chen, S. Fritzsche, S. Schippers, H. B. Wang, S. X. Wang, C. Liu, W. L. Ma, X. P. Zhou, M. Y. Wan, L. J. Mao, J. Li, M. T. Tang, K. Y. Yan, Y. B. Zhou, Y. J. Yuan, J. C. Yang, S. F. Zhang, L. F. Zhu, X. Ma
Figure caption: Plasma recombination rate coefficients of Na-like Fe15+. (a) The comparison of plasma rate coefficients between experimental results (black line) and the AUTOSTRUCTURE (red line), FAC (blue dashed and blue line), and JAC (orange dashed–dotted line) results in this work. The error bars denote the ±30% experimental uncertainty of the absolute rate coefficients. (b) Comparison of field-ionization-free plasma recombination rate coefficients (light-gray area) with theoretical data available in the literature. Full squares and triangles represent rate coefficients by M. Arnaud & J. Raymond (1992) and P. Mazzotta et al. (1998), respectively. Results from M. F. Gu (2004) and Z. Altun et al. (2006) are depicted by filled circles and stars, respectively. Full hexagons represent early experiment rate coefficients by S. Schippers et al. (2010). The temperature ranges associated with photoionized and collisionally ionized plasmas, where the Fe15+ concentration exceeds 10% of its maximum abundance, are indicated following P. Bryans et al. (2009) and T. Kallman & M. Bautista (2001).
Paper: Absolute Rate Coefficients for Dielectronic Recombination of Sodium-like Iron Ions: Experiment and Theory
Authors: H. K. Huang, W. Q. Wen, Z. K. Huang, Y. Yuan, C. Y. Zhang, R. Si, S. J. Wu, C. Y. Chen, S. Fritzsche, S. Schippers, H. B. Wang, S. X. Wang, C. Liu, W. L. Ma, X. P. Zhou, M. Y. Wan, L. J. Mao, J. Li, M. T. Tang, K. Y. Yan, Y. B. Zhou, Y. J. Yuan, J. C. Yang, S. F. Zhang, L. F. Zhu, X. Ma
Figure caption: Experimental DR rate coefficients (black filled symbols) for Na-like Fe15+ are presented across the electron–ion collision energy range of 0–40 eV. DR series associated with 3s → 3p and 3s → 3d core excitations (Δn = 0) are observed, with their resonance positions indicated by vertical colored bars. The theoretical DR rate coefficients from the AUTOSTRUCTURE, FAC, and JAC codes are depicted by the red, blue, and orange lines, respectively. These theoretical curves account for recombination into Rydberg states, with principal quantum numbers extending up to n = 1000, 300, and 300, respectively, representing the field-ionization-free recombination rate coefficient.
Paper: Absolute Rate Coefficients for Dielectronic Recombination of Sodium-like Iron Ions: Experiment and Theory
Authors: H. K. Huang, W. Q. Wen, Z. K. Huang, Y. Yuan, C. Y. Zhang, R. Si, S. J. Wu, C. Y. Chen, S. Fritzsche, S. Schippers, H. B. Wang, S. X. Wang, C. Liu, W. L. Ma, X. P. Zhou, M. Y. Wan, L. J. Mao, J. Li, M. T. Tang, K. Y. Yan, Y. B. Zhou, Y. J. Yuan, J. C. Yang, S. F. Zhang, L. F. Zhu, X. Ma
Figure caption: Similar to Figure 1 but for the electron–ion collision energy range of 40–90 eV. In this energy range, the contributing DR resonances are 3dnℓ(n ≥ 9) and ﹩4\ell 4{\ell }^{{\prime} }﹩ states. The JAC results near the limit of 3dnℓ are multiplied by a factor of 2. For further details, refer to the main text.
Paper: Absolute Rate Coefficients for Dielectronic Recombination of Sodium-like Iron Ions: Experiment and Theory
Authors: H. K. Huang, W. Q. Wen, Z. K. Huang, Y. Yuan, C. Y. Zhang, R. Si, S. J. Wu, C. Y. Chen, S. Fritzsche, S. Schippers, H. B. Wang, S. X. Wang, C. Liu, W. L. Ma, X. P. Zhou, M. Y. Wan, L. J. Mao, J. Li, M. T. Tang, K. Y. Yan, Y. B. Zhou, Y. J. Yuan, J. C. Yang, S. F. Zhang, L. F. Zhu, X. Ma
Figure caption: The fitting of the first four experimental resonance peaks at relative energies below 2.5 eV, as described in the reference by Z. K. Huang et al. (2018). The experimental DR rate coefficient and peak fitting are shown by the black filled symbols and the solid magenta line. The individual fitted peaks are shown by dash blue lines. The fit resulted in kBT∥ = 0.12(1) and kBT⊥ = 36.2(2) meV.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Convergence of gravitational waveform for the calibration binary black hole run. Top: we show the real part of the quadrupolar (ℓ = m = 2) component of Ψ4 from the high-resolution run, and in colored lines we show the residual between mid and low resolution ﹩| {{\rm{\Psi }}}_{4}^{{\rm{mid}}}-{{\rm{\Psi }}}_{4}^{{\rm{low}}}| ﹩ (in purple), and between high and mid resolution ﹩| {\Psi }_{4}^{\mathrm{high}}-{\Psi }_{4}^{\mathrm{mid}}| ﹩ (in orange). To demonstrate fourth-order convergence, we scale up the residual between the high and mid resolution by the Q factor defined in Equation (11) and plot it as a dashed cyan curve. When this curve is compared with the purple curve, clear fourth-order convergence is seen. Bottom: the same but for the phase difference between the waveforms.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Comparison of error in gravitational waveform with different grid structures. The error is estimated by taking the difference between the waveform of a given run and that for the high-resolution run. The Mid (blue) and Low (orange) Lev 10 runs share the same mesh refinement structure, yet the Mid has twice the resolution within each MeshBlock. Low Lev 11 (red) has the same root grid as Low Lev 10, yet one more level of mesh refinement, yielding the same resolution at the puncture as the mid-resolution run. We find that during the inspiral phase Low Lev 11 yields an error consistent with the Mid Lev 10 run, despite being roughly 8 times cheaper.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Mesh refinement structure during the calibration binary black hole run using the χ criterion. The history of punctures’ location (through puncture trackers) is overplotted as blue and red curves.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Waveform comparison between AthenaK and GR-Athena++. As in Figure 10, the black curve shows the waveform amplitude at high resolution from AthenaK. The purple and orange curves show the difference between the two codes for the low- and mid-resolution runs, respectively.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Weak-scaling performance (top) and efficiency (bottom) for evolving a single black hole on Frontier and Aurora with varying MeshBlock sizes.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Strong-scaling performance (top) and efficiency (bottom) for evolving a single black hole with 643 MeshBlock on both Frontier and Perlmutter.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: Amplitude of guider error signals in closed-loop guiding on the 38 Dra calibration field at an altitude of ≈107,000 feet. The different guidance phases plotted include the initial transition into closed loop, the guider system commanding a pointing offset, a performance window of on-target guidance, and a guider camera focus scan.