adsabs/AstroCLIMB huggingface dataset:
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Example PSF-matched image sets for NGC 0628. These image sets span the FUV to IR (see annotations) and have been convolved to Gaussian PSFs with FWHM values of 6″ (top row) and 40″ (bottom row). The red ellipse estimates the K  s -band 20 mag arcsec−2 isophotal contours. We used such apertures, along with the 40″ FWHM PSF image sets to extract galaxy-integrated photometry for FUV-to-FIR data sets. For 27 galaxies, we made use of the 6″ FWHM PSF image sets to extract much smaller photometry associated with the galaxy centers, where we exclude X-ray data and local SFH contributions from our analyses. For NGC 0628, we excluded a very small 6″ diameter circular region from our analysis (not shown here due to its relatively small size).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: False-color optical/near-IR postage-stamp images for the 88 galaxies in our sample. The observatories used to create these postage stamps vary, but are mainly based on ﹩g^{\prime} ﹩ (blue), ﹩r^{\prime} ﹩ (green), and ﹩i^{\prime} ﹩ (red) band data from SDSS or Pan-STARRS. Other postage stamps are based on best-matched filters from CTIO, KPNO, Swift UVOT, or HST data. Image sizes are square in dimensions and have manually determined scales ranging from 0.3 to 1.3 ×(2a), where a is the semimajor axis provided in Table 1. A 1′ length vertical gray bar is provided in the lower-right corner of each image for scale.
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Best-fit age- and metallicity-dependent power-law fit parameters, based on the model defined in Equations (13) and (14). These results constrain breaks and cutoff luminosities for the XRB XLFs (bottom panel) and indicate that (1) the XLF normalization, A, declines with age at a pace that is slower for lower-metallicity galaxies; (2) that the low-luminosity slope, α 1, becomes shallower with increasing age; and (3) the medium- and high-luminosity XLF slopes, α 2 and α 3, increase with increasing age with lower-metallicity galaxies having shallower high-L XLF slopes.
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Galaxy-integrated intrinsic 0.5–8 keV luminosity, L X, vs. SFR for main-sequence and starburst galaxies in our sample (filled circles with 1σ error bars). SFR values were calculated from our SED fitting posterior distributions (see Section 3), and L X was calculated from our broken power-law XLF modeling procedure (see Section 4) and Equation (9). Our best-fit linear regression model to these data is shown as a solid-black line (see Equation (10)) and comparisons from the literature are shown (see annotations).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: XLF model-integrated L X/M ⋆ as a function of age for five metallicity bins (see annotations in the upper right of each panel). The black curves (line styles varying by metallicity) and gray bands indicate median and 16%–84% ranges, respectively. The lower-right panel shows models for all five metallicity bins together for comparison. We overlay comparisons of the binary population synthesis models from T. Fragos et al. (2013b; dotted magenta curves), the Chandra Deep Field statistical constraints for z ≈ 0–2 normal galaxies from W. Gilbertson et al. (2022; blue-filled circles in the 0.5 Z ⊙ panel), subgalactic constraints in M51 from B. D. Lehmer et al. (2017; green-filled squares in the 1.5 Z ⊙ panel), and average L X/M ⋆ values for elliptical galaxies from B. D. Lehmer et al. (2020; red-filled triangle in the 1.5 Z ⊙ panel).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: XLF model-integrated L X/SFR vs. metallicity for young stellar populations (<100 Myr), as calculated using Equation (19) (solid black curve with gray envelope representing the 16%–84% confidence region). The observed quantities for the 63 main-sequence and starburst galaxies in our sample are shown as filled dark-gray circles with 16%–84% confidence intervals error bars. For comparison, we overlay the observation-based relations derived from M. Brorby et al. (2016; short-dashed blue) and E. Kyritsis et al. (2024; long-dashed gold), as well as the mean constraint for a sample of 30 high-z analogs from B. D. Lehmer et al. (2022; red-filled star), the X-ray stacking constraints and best-fit relation from F. M. Fornasini et al. (2019, 2020; filled-green squares and green dotted curve), and the binary population synthesis constraint from T. Fragos et al. (2013b; long-dashed magenta).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: (First 15 panels) Comparison of 15 derived parameters from SED fitting assuming BPASS (abscissa axes) and PÉGASE (ordinate axes). Parameter names are annotated in the upper left-hand corner of each plot; parameter definitions can be found in Table 3 and Section 5.3. In each panel, we further annotate the mean parameter ratios (BPASS/PÉGASE) and their 1σ uncertainties. We find near-unity agreement for several parameters with the exception of ψ 1 and ψ 6–ψ 8, which deviate by several sigma. (Final panel) Distribution of the logarithm of the posterior probability ratio (PÉGASE/BPASS) for the full sample. The distribution skews to values greater than zero, indicating that PÉGASE-based fits provide better characterizations of the SEDs in our sample.
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Best-fit stellar mass normalized integrated XLF models from Equations (13) and (14) separated into the 10 SFH age bins, as defined by our SED fitting (see Table 3), and evaluated at 5 metallicity bins per age bin (see annotations). Note that the first age bin shows no XLF curves due to our definition of A(t 9 < 0.03, Z) = 0 in Equation (14).
Paper: An Empirical Framework Characterizing the Metallicity and Star-formation History Dependence of X-Ray Binary Population Formation and Emission in Galaxies
Authors: Bret D. Lehmer, Erik B. Monson, Rafael T. Eufrasio, Amirnezam Amiri, Keith Doore, Antara Basu-Zych, Kristen Garofali, Lidia Oskinova, Jeff J. Andrews, Vallia Antoniou, Robel Geda, Jenny E. Greene, Konstantinos Kovlakas, Margaret Lazzarini, Chris T. Richardson
Figure caption: Distribution of simulated values of ﹩{C}_{\mathrm{sim}}﹩, as obtained from the MC procedure described in Section 5.3. Our best-fit value of C global is represented as a vertical red-dashed line, which indicates that such a value is consistent with the expected distribution from our simulations.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Measurements of the H − K′ spectral index/color of Sgr A*-NIR plotted against the measured magnitude in ﹩K^{\prime} ﹩. The Strehl ratio cuts, confusion correction, and interpolation filters have been applied. The dashed black lines show the location of the magnitude cuts for the bright subset and the extended data set. The dotted gray line corresponds to ﹩{m}_{H}^{\mathrm{est}}=20.3﹩, which is our estimate for the 50% completeness limit. The plotted uncertainties on α do not include the systematic error from the color excess, which is shown separately for reference. The data points plotted here are also available as a machine-readable table.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Flowchart representing the empirical model described in Section 4, relating the measured spectral index (﹩{\alpha }_{H-K^{\prime} }^{\mathrm{est}}﹩) to the measured magnitude in the ﹩K^{\prime} ﹩ band (﹩{m}_{K^{\prime} }^{\mathrm{est}}﹩). The free model parameters are highlighted in red. In green, we show the random variables that are sampled to account for noise. The equations constituting the model are gathered below the flowchart. Subscript/superscript “est” denotes the measured quantities (with noise), “obs” the quantities at the observer location (i.e., without noise, but not corrected for extinction), “SgrA” denotes the quantities for Sgr A*-NIR alone, and “bck” for the background alone. The following values are fixed: ﹩\langle E(H-K^{\prime} )\rangle =2.07﹩ for the mean color excess of Sgr A* (see Section 3.1), and κ = 0.0077, ﹩E{\left(H-K^{\prime} \right)}_{* }=2.09﹩ for the color excess law (see Appendix C).
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Top row: example images in ﹩K^{\prime} ﹩ (red) and H (blue) from 2022 May 21, zoomed-in on a 1″ × 1″ box around Sgr A*, showcasing its large variations in brightness. The bright nearby stars S0-2 and S0-6 (﹩{m}_{K^{\prime} }\sim 14﹩, m  H  ∼ 16) are labeled for reference. Bottom panel: Sgr A*-NIR lightcurves in the H and ﹩K^{\prime} ﹩ bands for the same epoch, interpolated using the method described in Section 3.3. The green arrows show which points in the lightcurve are selected by the interpolation filters to serve for the color/spectral index measurements. The black arrows indicate the location of the four images in the panels above.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison of the confusion-corrected (red) and uncorrected (gray) spectral index measurements of Sgr A*-NIR for the epochs when it is known to be confused (i.e., all except 2019 May 13). Uncorrected spectral index values are systematically bluer and brighter, moving toward stellar values (α * ∼ 2) when Sgr A*-NIR becomes faint. This trend disappears after applying confusion correction. Note that here the plotted spectral index uncertainties do not include the systematic error from the color excess, which is shown separately for reference.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison of the uncorrected (gray) and confusion-corrected (red) lightcurves for 2022 August 19. The inset shows the posterior on the predicted position (relative to Sgr A*) of the star S0-38 confused with Sgr A*-NIR, inferred from orbital fits to long-term GC astrometric data (see Appendix D.1).
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison between the spectral index constraints obtained in this work and values found in other photometric studies in the NIR. The confidence intervals were obtained by sampling model parameters from the posterior plotted in blue in Figure 8 (i.e., from the extended data set, with ξ = 0), then computing the spectral index with zero noise. Points indicate individual measurements, and dotted lines the best-fit values over some range, when measurements were found to be consistent with a constant spectral index. Filled circles specify when color measurements between H and ﹩K^{\prime} ﹩ (or K) bands are used to determine the spectral index, open circles when other methods or NIR bands are considered. We show the systematic error from extinction correction separately; changing the color excess would shift our entire posterior distribution up/down.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Predicted distribution of H − K′ spectral index measurements at each measured magnitude in ﹩K^{\prime} ﹩, for a fixed set of model parameters  θ    s  . The contours are obtained by assuming some noise properties (here, Equation (1) with the mean values for ﹩{\mathrm{log}}_{10}({C}_{\mathrm{band}})﹩ and β band displayed in Table 3), and sampling ∼105 noise realizations for each measured magnitude ﹩{m}_{K^{\prime} }^{\mathrm{est}}﹩. Three examples are presented, illustrating the various physical pictures discussed in Section 4: (a) a constant spectral index for Sgr A*-NIR, with a faint stellar background, (b) a spectral index for Sgr A*-NIR varying linearly (with a slope ξ = 1.23) as a function of magnitude, on top of a faint stellar background, and (c) a two-state model of Sgr A*-NIR, with a constant spectral index for the flaring state, transitioning into a redder value for the quiescent state. We warn that the contours do not represent a joint 2D distribution on ﹩({m}_{K^{\prime} }^{\mathrm{est}},{\alpha }_{H-K^{\prime} }^{\mathrm{est}})﹩, but rather a normalized conditional distribution on ﹩{\alpha }_{H-K^{\prime} }^{\mathrm{est}}﹩ given a value ﹩{m}_{K^{\prime} }^{\mathrm{est}}﹩.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison between the actual H − K′ spectral index measurements from the full data set (in black) and the predicted distribution of ﹩{\alpha }_{H-K^{\prime} }^{\mathrm{est}}﹩ at each measured magnitude in ﹩K^{\prime} ﹩ (green). The contours are obtained similarly to Figure 6, i.e., by assuming some noise properties (here, Equation (1) with the mean values for ﹩{\mathrm{log}}_{10}({C}_{\mathrm{band}})﹩ and β band displayed in Table 3) and sampling ∼105 noise realizations for each measured magnitude ﹩{m}_{K^{\prime} }^{\mathrm{est}}﹩. This time, however, the model parameters  θ    s   are not fixed (except for ξ = 0), but sampled simultaneously from the posterior shown in blue in Figure 8. The red line indicates the best estimate for the constant spectral index (﹩\alpha =\hat{\eta }=-0.50﹩; see Figure 8). The systematic error from the color excess is shown separately, since changing the value of ﹩\langle E(H-K^{\prime} )\rangle ﹩ would simply shift every spectral index by the same amount.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Joint posterior distribution of the constant spectral index η and the background parameters (﹩{m}_{K^{\prime} }^{\mathrm{bck}},{\alpha }_{\mathrm{bck}}﹩), assuming a model with fixed slope ξ = 0, for the bright subset (in black) and the extended data set (in blue). The magnitude of the background is completely unconstrained when ﹩{\alpha }_{\mathrm{bck}}\approx \hat{\eta }=-0.50﹩, since in that case background and main emission would be impossible to distinguish with two-band photometry. The contours have been smoothed slightly for visualization purposes.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison between the spectral index constraints obtained in this work and values found in spectroscopic studies in the NIR. Open (resp. filled) circles denote measurements with (resp. without) precursor/off-state substraction, a method that can bias spectral index measurements by removing flux that should be attributed to Sgr A*-NIR.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Color excess ﹩\hat{E}(H-K^{\prime} )﹩ from Equation (C3), obtained by setting ﹩{\alpha }_{H-K^{\prime} }^{\mathrm{meas}}={\alpha }_{\mathrm{int}}﹩ in Equation (C2), as a function of the intrinsic spectral index α int of the source, for different extinction curves. We show three examples consistent with the values from T. K. Fritz et al. (2011): A 0 = A 2.166μm = 2.62 ± 0.11, β = 2.11 ± 0.06, and compare them to a linear relation with a fitted slope κ ≈ 0.008.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Example of synthetic frame construction in star-planting simulations. Here, the observed frame used as a reference is the first ﹩K^{\prime} ﹩ frame of 2022 May 21. From left to right, the panels show 0.″8 × 0.″8 cutouts around Sgr A* of (a) the simulated source representing Sgr A*-NIR (planted with m plant = 16.8), (b) one realization of the simulated source representing S0-38, the confused star (sampling the magnitude and position from known distributions), (c) the background and other sources found by StarFinder in the observed image, and (d) the final synthetic frame (summing the previous contributions and adding white noise).
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Joint posterior distribution of ξ and η, inferred from the bright subset in black, from the extended data set in blue (see Figure 4), and marginalized over the background parameters (﹩{m}_{K^{\prime} }^{\mathrm{bck}},{\alpha }_{\mathrm{bck}}﹩). The contours have been smoothed slightly for visualization purposes. The red line shows ξ = 0.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Weighted standardized mean square error for the median estimator, as a function of Strehl ratio, for a reference star in each band. The red dashed lines indicate the chosen threshold values for the Strehl ratio cuts.