adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: A summary of simulation results from the IWG showing how β is a function of assumed yield strength (cohesion, Y0) and target porosity (φ). Individual simulations are plotted as circles and colored by the calculated value for β. In cases where more than one simulation is plotted in the same parameter space, the simulation with the highest β is plotted on top. Dashed horizontal lines are plotted for the range of porosity values possible based on the current DART project Design Reference Asteroid (DRA), the “DRA” value represents the currently assumed most likely porosity. The vertical lines show representative potential strength values, including the transition where crater scaling changes from gravity to strength. Dynamical considerations suggest Dimorphos could be as weak as 10 Pa. The line at *** represents the strong end-member for meteorite strengths calculated by Cotto-Figueroa et al. (2016).
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: Resulting ε from hypervelocity impact simulations into solid basalt targets, the offset vector of ejecta from the surface normal direction can be affected by impact geometry and material properties of Dimorphos. Though expected to be small, this offset can provide information about the porosity (left) and material strength (middle) of Dimorphos. (right) The momentum enhancement factor (β) is also affected by the angle at which material is ejected from the surface. Note these represent offsets of only ∼6°–10° for Spheral calculations and up to ∼20° for the CTH calculations shown here.
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: Parallel-line plot from a subset of iSALE simulations showing the relationship between porosity (φ), coefficient of friction (fi) and material strength/cohesion (Y0), and the resulting momentum enhancement. The lines are colored by the value of β. A range of material property combinations can produce similar momentum enhancement.
Paper: Effects of Impact and Target Parameters on the Results of a Kinetic Impactor: Predictions for the Double Asteroid Redirection Test (DART) Mission
Authors: Angela M. Stickle, Mallory E. DeCoster, Christoph Burger, Wendy K. Caldwell, Dawn Graninger, Kathryn M. Kumamoto, Robert Luther, Jens Ormö, Sabina Raducan, Emma Rainey, Christoph M. Schäfer, James D. Walker, Yun Zhang, Patrick Michel, J. Michael Owen, Olivier Barnouin, Andy F. Cheng, Sidney Chocron, Gareth S. Collins, Thomas M. Davison, Elisabetta Dotto, Fabio Ferrari, M. Isabel Herreros, Stavro L. Ivanovski, Martin Jutzi, Alice Lucchetti, Elena Martellato, Maurizio Pajola, Cathy S. Plesko, Megan Bruck Syal, Stephen R. Schwartz, Jessica M. Sunshine, Kai Wünnemann
Figure caption: Crater morphologies from iSALE-2D impact simulations of DART-like impacts into targets with a variety of material properties and structures that produce very similar β values.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Rim-to-rim crater diameter (a) and momentum enhancement β (b) for increasing impact velocity for regolith simulant. The numerical results are listed in Table 3. The projectile mass was 24 mg. The experimental velocity range was extended above 2.5 km s−1 into the DART regime. Colors indicate a variation in the coefficient of friction. The results for crater size scaling in the strength regime (panel a) are given according to Housen & Holsapple (2011), including the densities of projectile and target, and using the scaling exponent ν = 0.3. The scaling exponent μ = 0.37 (dashed gray line) was derived from fitting procedures for ejection velocities as described by Luther et al. (2018). The scaling factor is H2 = 0.55, and the effective strength was set to the value for the cohesion. The gray line in panel (b) shows the estimated dependence of β from the impact velocity v Pr from Chourey et al. (2020): ﹩\beta =1+0.15\ {v}_{{\Pr }}^{0.92}﹩. The dashed black line shows our fit: ﹩\beta =1+0.21\ {v}_{{\Pr }}^{0.7}﹩. The velocity exponent can be translated into the scaling exponent μ by the following relation (Holsapple & Housen 2012): ﹩\beta \sim 1+{v}_{{\Pr }}^{3\mu -1}﹩, which gives values of μ = 0.64 and μ = 0.56 for both relations, respectively.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Cumulative ejecta mass over launch velocity for the benchmark scenarios, a DART-like impact into regolith targets, for iSALE (solid lines), Bern SPH (dotted lines), and miluphcuda (dashed lines). Results are plotted for 20% and 50% porosity, as well as all three cohesions in panels (a), (b), and (c). Panel (d) combines all three cohesions for a single porosity of 20%. Colors represent the material porosity (a–c) or cohesion (d). m0 and v0 are the impactor mass (600 kg) and velocity (6 km s−1), respectively.
Paper: After DART: Using the First Full-scale Test of a Kinetic Impactor to Inform a Future Planetary Defense Mission
Authors: Thomas S. Statler, Sabina D. Raducan, Olivier S. Barnouin, Mallory E. DeCoster, Steven R. Chesley, Brent Barbee, Harrison F. Agrusa, Saverio Cambioni, Andrew F. Cheng, Elisabetta Dotto, Siegfried Eggl, Eugene G. Fahnestock, Fabio Ferrari, Dawn Graninger, Alain Herique, Isabel Herreros, Masatoshi Hirabayashi, Stavro Ivanovski, Martin Jutzi, Özgür Karatekin, Alice Lucchetti, Robert Luther, Rahil Makadia, Francesco Marzari, Patrick Michel, Naomi Murdoch, Ryota Nakano, Jens Ormö, Maurizio Pajola, Andrew S. Rivkin, Alessandro Rossi, Paul Sánchez, Stephen R. Schwartz, Stefania Soldini, Damya Souami, Angela Stickle, Paolo Tortora, Josep M. Trigo-Rodríguez, Flaviane Venditti, Jean-Baptiste Vincent, Kai Wünnemann
Figure caption: Coordinate system and angles. (a): The tan square in perspective indicates the asteroid surface around the point of impact, with the darker semicircle suggesting subsurface material that will be excavated and ejected. The spacecraft arrives traveling in the ﹩-z^{\prime} ﹩-direction, at an impact angle i from the surface normal ﹩\widehat{{\boldsymbol{n}}}﹩. The net momentum of the outgoing unbound ejecta, in the homogeneous case, is coplanar with z′ and ﹩\widehat{{\boldsymbol{n}}}﹩, and directed at an ejection angle α from the normal. (b): As in (a), showing the parameterization of the random part of the response. The ejecta momentum is increased in magnitude by a factor (1 + ζ) and altered in direction by an angle ξ at azimuth θ.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Validation results for iSALE, Bern SPH, and miluphcuda in regolith simulant targets. The top panel (a) shows results for surface crater diameters, the bottom panel (b) for β. The data are listed in Table 2. The error bars in the top panel do not refer to experimental uncertainties; instead, they estimate the uncertainty in converting rim–rim diameters (as measured by Chourey et al. 2020) to pre-impact surface diameters. The upper limits of the bars correspond to a ratio of D rim/D surf = 1, while the lower limits indicate D rim/D surf = 1.3 (as stated by Housen & Holsapple 2011). For our simulations, we inferred a most probable factor of ∼1.15, based on our iSALE models.
Paper: After DART: Using the First Full-scale Test of a Kinetic Impactor to Inform a Future Planetary Defense Mission
Authors: Thomas S. Statler, Sabina D. Raducan, Olivier S. Barnouin, Mallory E. DeCoster, Steven R. Chesley, Brent Barbee, Harrison F. Agrusa, Saverio Cambioni, Andrew F. Cheng, Elisabetta Dotto, Siegfried Eggl, Eugene G. Fahnestock, Fabio Ferrari, Dawn Graninger, Alain Herique, Isabel Herreros, Masatoshi Hirabayashi, Stavro Ivanovski, Martin Jutzi, Özgür Karatekin, Alice Lucchetti, Robert Luther, Rahil Makadia, Francesco Marzari, Patrick Michel, Naomi Murdoch, Ryota Nakano, Jens Ormö, Maurizio Pajola, Andrew S. Rivkin, Alessandro Rossi, Paul Sánchez, Stephen R. Schwartz, Stefania Soldini, Damya Souami, Angela Stickle, Paolo Tortora, Josep M. Trigo-Rodríguez, Flaviane Venditti, Jean-Baptiste Vincent, Kai Wünnemann
Figure caption: Constraints on the ejecta response (η, α) obtained from a hypothetical measurement, β  p  = 2.1, for the DART kinetic impact. The local density of small black points is proportional to the likelihood that the corresponding (η, α) pair reproduces the measured β  p . (a): Homogeneous case, with no surface irregularities. (b): Including the random effect of surface irregularities. The vertical dashed line corresponds to ejecta momentum normal to the surface. The colored points indicate predictions from hydrodynamic simulations, as in Figure 3.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Benchmark results for all three codes in regolith targets for a DART-like impact. Results for iSALE-2D are shown by hollow symbols, and the trend is indicated by solid lines. Results for Bern SPH are shown by filled symbols, and the trend is indicated by dashed lines. Colors represent the material cohesion. The 600 kg impactor has a velocity of 6 km s−1.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Scaling exponent μ as function of porosity for regolith simulant with a cohesion of 1.4 kPa (top), 10 kPa (middle), and 100 kPa (bottom), and a coefficient of friction of 0.77. The gray symbols denote: diamond—weakly cemented basalt, triangle—sand, plus—glass microspheres, and cross—sand/fly ash as derived by Housen & Holsapple (2011 and references therein). The colors represent the shock physics code. The uncertainty is about the size of the symbols (+/−0.01). Only for the 100 kPa cohesion is the uncertainty slightly larger (+/−0.02), due to the smaller power-law regime. The black circles show the average values.
Paper: Momentum Enhancement during Kinetic Impacts in the Low-intermediate-strength Regime: Benchmarking and Validation of Impact Shock Physics Codes
Authors: Robert Luther, Sabina D. Raducan, Christoph Burger, Kai Wünnemann, Martin Jutzi, Christoph M. Schäfer, Detlef Koschny, Thomas M. Davison, Gareth S. Collins, Yun Zhang, Patrick Michel
Figure caption: Crush curves for the same regolith material using two different porosity compaction models: ε–α (iSALE) and P–α (both SPH codes). All parameters are given in Table 4. The left panel shows the pressure–distension relation, and the right panel shows the same for a normalized distension.
Paper: Probing the Icy Shell Structure of Ocean Worlds with Gravity–Topography Admittance
Authors: Ryunosuke Akiba, Anton I. Ermakov, Burkhard Militzer
Figure caption: Snapshot of the flow within a 21 km shell of Enceladus driven by the viscous relaxation of an artificial mountain. A large axially symmetric mountain, expressed as a Gaussian (﹩R+{{he}}^{-2.5{\theta }^{2}}﹩ for height h, colatitude θ, and FWHM of ≈60°), was placed at the pole and expanded in spherical harmonics. It was then relaxed under bottom material (A), (C) and bottom phase (B), (D) boundary conditions for a uniform-viscosity shell (A), (B) and a gradient-viscosity shell (C), (D). The gradient-viscosity shell has a viscosity contrast of η  t /η  b  = 108 Pa s with η  t  = 1022 Pa s. The streamlines represent the direction and colors represent the magnitude of the velocity of the ice flow found from our Stokes flow model. For viscous relaxation under the bottom material boundary, the snapshot was taken when the dominant motion in the shell is downwards (symmetric mode of relaxation). For the bottom phase boundary, the figure shows the state of dynamic equilibrium. The flow field is limited to within the spherical surfaces denoted by dashed curves. The reason for this is that we represent topography that drives the flow as loads, which generate stress and gravity perturbations on the spherical boundaries.
Paper: Probing the Icy Shell Structure of Ocean Worlds with Gravity–Topography Admittance
Authors: Ryunosuke Akiba, Anton I. Ermakov, Burkhard Militzer
Figure caption: Illustration of bottom material (left) and bottom phase (right) boundary conditions. The icy shell is shown with outer radius R and thickness D with some hypothetical topography (not to scale). ﹩{\boldsymbol{h}}={[{h}_{t},{h}_{b}]}^{T}﹩ are the shapes of the surface and base of the icy shell, v  r  is the radial velocity, and σ  rr  and σ  r θ  are the radial stress and poloidal shear stress perturbations. δ V is the gravitational potential perturbation. Note that the boundary conditions for the bottom material boundary are functions of time, while the bottom phase boundary is in dynamic equilibrium.
Paper: Probing the Icy Shell Structure of Ocean Worlds with Gravity–Topography Admittance
Authors: Ryunosuke Akiba, Anton I. Ermakov, Burkhard Militzer
Figure caption: Admittance spectra of Europa with a 30 km icy shell. We show admittance spectra with both (A) bottom material and (B) bottom phase boundary conditions for a range of viscosity gradients. Viscosity is assumed to decrease exponentially with depth, with the viscosity contrast from the surface to the base η  t /η  b , where η  b  = 1014 Pa s and is fixed. For the two high-viscosity contrasts, admittance spectra for a bounded viscosity η bound = 1022 Pa s are shown. The uniform-viscosity case (η  t /η  b  = 1) is plotted in purple. Admittance spectra assuming uncompensated topography and Airy isostasy are shown by the black dashed and dotted curves, respectively.
Paper: Probing the Icy Shell Structure of Ocean Worlds with Gravity–Topography Admittance
Authors: Ryunosuke Akiba, Anton I. Ermakov, Burkhard Militzer
Figure caption: Effects of tidal heating on temperature and viscosity in a 30 km shell of Europa. (A) Conductive temperature profiles converged from the iterative process for a melting point viscosity η melt = {1013, 1014} Pa s and for a case without tidal heating (h tide = 0). (B) Unbounded temperature-dependent viscosity profiles calculated from the temperature profiles of (A) with Equation (2). The viscosity at which Maxwell time is crossed is shown by the red dotted line. The case without tidal heating is shown for both choices of η melt. (C) Surface-averaged volumetric tidal dissipation rate is shown for η melt = {1013, 1014} Pa s. Maximum tidal dissipation can be seen occurring at the depth where the viscosity profile crosses η Maxwell.
Paper: Probing the Icy Shell Structure of Ocean Worlds with Gravity–Topography Admittance
Authors: Ryunosuke Akiba, Anton I. Ermakov, Burkhard Militzer
Figure caption: Flowchart for our exploration of the icy shell structure.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: (a)–(b) Surface maps for IS in the south and north, respectively. The IS surface maps are based on measurements of the northern cusp by the MESSENGER FIPS instrument (Raines et al. 2014). They are only used as a reasonable basis for illustrating the differences resulting from the different SBE values, and are not necessarily reflective of actual open cusp areas at Mercury, especially in the southern hemisphere where similar measurements are not available. (c) Source map for PSD. The scaling is informed by fits to the MESSENGER MASCS data and diffusion-limited supply (Burger et al. 2010).
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: These simulations trace the gradual change in the exosphere derived from IS, from the northern cusp only, assuming SBEs of (a) 0.27 eV, (b) 2.6 eV, (c) 4.4 eV, and (d) 7.9 eV. The +x-axis is toward the Sun and +z is northward. Column density is the cumulative number of atoms cm−2 along the line of sight in the y-axis direction, which runs dawn–dusk and is perpendicular to the page.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: The IV-generated exosphere is simulated for the (a) lower limit and (b) upper limit from Mouawad et al. (2011). The image is seen from the dawn hemisphere centered on the terminator. The Sun is to the right and north is up.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Altitude profiles measured radially from the planet directly above the center of the cusp at a latitude of 67°N. Four values of SBE were assumed: 0.27, 2.6, 4.4, and 7.9 eV. The plots have been smoothed, but the high altitudes still appear wavy owing to poor statistics. Above about 1000 km the curves asymptote because all trajectories are escaping.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Comparisons of our models to MESSENGER data. The column density shown is an integrated line-of-sight value, not a zenith column. The data (black circles) are subsolar MESSENGER MASCS limb scan data at TAA 144° from Cassidy et al. (2015; upper-right panel of their Figure 6). The green regions indicate the range of PSD altitude profiles, with the lower edge corresponding to a PSD cross section of 1 × 10−20 cm2 and f Na = 0.02 (which we take as lower limits of both parameters), and the upper edge corresponding to the measured PSD cross section of 3 × 10−20 cm2 and f Na = 0.05 (we take as upper limits of both parameters). The orange regions indicate the range of IV altitude profiles, with the lower edge corresponding to the minimum IV case (1 × 105 cm−2 s−1) and the upper edge to the maximum IV case (2.1 × 106 cm−2 s−1) at 0.352 R  h  of Mouawad et al. (2011). IV is always scaled as R  h  −2. The blue curves indicate the sum of the altitude profiles from IS in both the north and south cusps for SBE = 0.27 eV (a) and SBE = 7.9 eV (b) with an assumed flux equal to the MESSENGER FIPS-measured maximum (6.7 × 108 ions cm−2 s−1; Raines et al. 2014). The red curves are example combinations of PSD, IV, and IS that match the data (see text for discussion). The red curve in (a) is the sum of PSD for the enhanced cross section and f Na = 0.04, IV for the maximum case, and 0.03 times the blue curve for the IS contribution (i.e., a flux of 2.0 × 107 ions cm−2 s−1). The red curve in (b) is the sum of PSD for the enhanced cross section and f Na = 0.04, IV for the maximum case, and the blue curve for the IS contribution.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: (a) PSD seen from the dawn equatorial terminator. (b) Maximum IV spot at dawn combined with IS at the northern cusp only and SBE = 0.27 eV. This provides an illustration of a single cusp being open to the solar wind. (c) Same as (b) but with SBE = 7.9 eV.
Paper: The Influence of Surface Binding Energy on Sputtering in Models of the Sodium Exosphere of Mercury
Authors: Rosemary M. Killen, Liam S. Morrissey, Matthew H. Burger, Ronald J. Vervack, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Comparison of the combination of IS (from both the northern and southern cusp) and IV, in which the simulation in Figure 4 for minimum IV flux has been added to IS exospheres for SBEs of (a) 0.27 eV, (b) 2.6 eV, (c) 4.4 eV, and (d) 7.9 eV. These illustrate where and to what extent the two processes can be distinguished.
Paper: Detecting Lipids on Planetary Surfaces with Laser Desorption Ionization Mass Spectrometry
Authors: Nikita J. Boeren, Salome Gruchola, Coenraad P. de Koning, Peter Keresztes Schmidt, Kristina A. Kipfer, Niels F. W. Ligterink, Marek Tulej, Peter Wurz, Andreas Riedo
Figure caption: Left: concentration scans of 17α-ethynylestradiol, phylloquinone, and α-tocopherol with observed peak area to surface area concentration [fmol mm−2]. The linear regression line (y = a + bx, where y = log(Peak Area) and x = log(Concentration)) for each lipid is also shown. Right: theoretical LODs for each investigated lipid given in fmol mm−2. The LOD value is obtained by extrapolating linear regression lines down to the 3σ noise level.