adsabs/AstroCLIMB huggingface dataset:
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Differences in vertical structure between the spatially averaged 1D MHD atmosphere and the RE models.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Comparison between relative contrasts computed from the MHD cube, RE models, and the Phoenix spectra for the M dwarfs.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Ratio of spot spectra from every cube used in our analysis to the spectra from the average of all the cubes, shown here for G, K, and M spectral types.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Same as Figure 7 but for a K0 dwarf.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: A comprehensive spatially resolved view of our galaxy sample with metallicity gradient measurements. For each galaxy, we show eight subplots on two rows. The first row displays, from left to right, the three-color image, Hα emission flux map, observed Hα velocity map, and intrinsic Hα velocity dispersion map (corrected for instrument resolution). The second row shows the gas-phase metallicity map using the N2 method, the metallicity gradient with the best linear fit represented by the red dashed line, a map color-coded according to the positions of individual spaxels in the BPT or WHAN diagram, and the BPT or WHAN diagram used to classify the ionization properties in each galaxy. The red boxes in the three-color images indicate the FoV (﹩1\mathop{.}\limits^{^{\prime\prime} }8\times (2\mathop{.}\limits^{^{\prime\prime} }0-3\mathop{.}\limits^{^{\prime\prime} }0)﹩) for each of our sources. The ellipses on the maps represent the size of the resolution element of our MSA-3D IFS. For subplots other than the metallicity maps and the metallicity gradients, we show spaxels with an S/N of flux(Hα) > 10 and an S/N of EW(Hα) > 5. For the metallicity maps and gradients, we plot only the subset of those spaxels classified as star-forming with a statistical uncertainty of <0.25 dex in metallicity. For the metallicity gradient subplots, the bottom and top abscissas are the galactocentric radius in units of kiloparsecs and effective radius Re, respectively. In these subplots, we report the best-fit metallicity gradient slope for each galaxy based on individual spaxels, along with the scatter (i.e., the RMSE between the metallicity of individual spaxels and the linear fit). The red points and error bars show the metallicity profiles using averages in radial bins.Instrumental color–magnitude diagram for cluster BS 121. (An extended version of this figure is available in the online article.)Instrumental color–magnitude diagram for cluster BS 121.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: Kinematic properties of galaxy ID 4391, with the complex chemical profile verified by different metallicity indicators. Panel (a): the NIRCam/F115W image stamp of galaxy ID 4391. Panel (b): the metallicity map obtained using the O3N2 method. Panels (c) and (d): metallicity gradients with galactocentric radii in units of kiloparsecs and Re units determined by the N2 method (red dots) and the O3N2 method (blue dots). The points and error bars show the metallicity profiles using averages in radial bins. The black line in the two panels represents the slope for local galaxies (F. Belfiore et al. 2017). Both methods display a distinct gradient from the galaxy center to the outskirts, with a turning point located near 2.5 Re. Panel (e): the 1D velocity profile (black and gray dots) with the best-fitting model shown in red. Panel (f): the 1D intrinsic velocity dispersion is presented on the same spatial axis as the velocity profile. The gray dots represent the intrinsic velocity dispersion, while the green error bars indicate the median and standard deviation of the gray dots within radial bins. The vc/σ is 1.91 ± 0.14, indicating irregular rotational motion and suggesting that this galaxy likely has a thick disk. The unusual metallicity profile might be attributed to galaxy mergers or gas inflows, both of which are also capable of significantly disturbing gas motions.
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Intensity maps of IRAS 23385+6053 at different wavelengths from the first, second, third, and fourth channels of the JWST MIRI-MRS spectrograph. The white circle shows 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 aperture from which the spectrum is extracted. Channels have different pixel size and map size depending on the observed wavelength. The YSOs are designated as A and B as in L. Francis et al. (2024). The white circle in the lower left corner shows the FWHM. The red circle shows the surface emission area of gaseous methane. The red cross shows the methane gas emission peak.
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Panel (a)—The IRAS 23385+6053 spectrum after background subtraction. Global continuum is adopted from W. R. M. Rocha et al. (2024). The inset shows a zoom-in on the 7.7 μm region. Panel (b)—A processed spectrum after global, local continuum, and a silicate profile subtraction. Panel (c)—Same as (b) but with non-CH4 ices (OCN−, CH3CH2OH, SO2) subtracted following W. R. M. Rocha et al. (2024).
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Top panel—the warm-up of the mixture CH4 : CO2 = 1 : 5 from 6.7 K and 10 K with 0.5 K per minute; bottom panel—the warm-up of the mixture CH4 : H2O = 1 : 10 from 6.7 K and 10 K with 0.5 K per minute. The CO2 mixture is seen to be strongly influenced by the deposition temperature. The dashed lines mark the peak positions for H2O mixtures observed before the warm-up and serve as visual guides.
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Best simulated gaseous methane spectrum plotted against observational data with subtracted ice continuum. A good agreement is shown between the prominent gaseous features and outlying sharp features in the observational spectrum.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: Correlations among the metallicity gradient, redshift, and stellar mass. Left: metallicity gradients as a function of redshift. The red points with 1σ error bars correspond to our results. The orange and blue lines correspond to the MUGS (“weak” feedback) and MAGICC (“enhanced” feedback) simulations from B. K. Gibson et al. (2013), respectively. The green line represents the predicted evolution of metallicity gradients from the TNG50 simulations (Z. S. Hemler et al. 2021), the magenta line shows predictions from the FIRE-2 zoom-in simulations (X. Sun et al. 2024a), and the yellow line corresponds to the results from EAGLE simulations (P. B. Tissera et al. 2022). The gray scale shows a density histogram derived from previous observational results in the literature at z = 0.5−3 (J. Queyrel et al. 2012; A. M. Swinbank et al. 2012; T. Jones et al. 2013; N. Leethochawalit et al. 2016; E. Wuyts et al. 2016; J. Molina et al. 2017; X. Wang et al. 2017, 2019, 2020, 2022b; D. Carton et al. 2018; N. M. Förster Schreiber et al. 2018; V. Patrìcio et al. 2019; M. Curti et al. 2020; R. C. Simons et al. 2021; Z. Li et al. 2022; G. Venturi et al. 2024). The gradients in our sample are flat and nearly redshift-invariant, showing higher values than those from the MUGS, MAGICC, and TNG50 simulations but similar to the results of the FIRE-2 zoom-in simulations. Right: metallicity gradients as a function of stellar mass. The red points represent our results, and the red line represents the best linear fit. The blue and green lines correspond to local galaxies (from F. Belfiore et al. 2017) and star-forming galaxies at cosmic noon (from Y. Cheng et al. 2024), respectively. The magenta line is the mass–metallicity gradient relationship predicted by the FIRE-2 simulations. The gray-scale density histogram in this panel is derived from results in the literature in the same range, z = 0.5−1.7, as our sample (J. Queyrel et al. 2012; A. M. Swinbank et al. 2012; N. Leethochawalit et al. 2016; E. Wuyts et al. 2016; J. Molina et al. 2017; X. Wang et al. 2017, 2019, 2020, 2022b; D. Carton et al. 2018; N. M. Förster Schreiber et al. 2018; V. Patrìcio et al. 2019; M. Curti et al. 2020; R. C. Simons et al. 2021). Our work reveals a mass dependence of metallicity gradients at ~2σ significance, showing that more massive galaxies exhibit more negative gradients, consistent with the FIRE-2 simulation results.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: Detailed spectroscopic and kinematic properties of galaxy ID 9960, the steepest gradient source in our sample. Panel (a): the spectrum from the spaxel in the galaxy center, with dashed lines highlighting the emission lines of Hβ, [O III], Hα, [N II], and [S II]. Hβ and [O III] unfortunately both fall within the chip gap. Panel (b): a zoomed-in spectrum of panel (a). The vertical dashed lines mark the wavelengths of Na I D λλ5890, 5896, Hα, [N II], and [S II]. The high flux ratio of [N II]/Hα and the strong blueshifted absorption of Na I D indicate the presence of AGN-driven outflows (e.g., M. A. Dopita et al. 1998; D. S. Rupke et al. 2005; R. L. Davies et al. 2024). Panels (c)–(e): image stamps of galaxy ID 9960 in the filters of HST/ACS F606W, JWST/NIRCam F115W, and JWST/NIRCam F356W. The red box marks the entire FoV of our slit-stepping 3D spectroscopy. Panel (f): the 1D velocity profile (black and gray dots) with the best-fitting model shown in red. The green dots represent the intrinsic velocity dispersion, corrected for the instrument line-spread function as described in the text. We derive vc/σ0 = 5.13 ± 0.20, which, together with the 2D velocity map (Figure A1), indicates that galaxy ID 9960 has a regularly rotating disk. The steep metallicity gradient and the clear rotation signatures of galaxy ID 9960 support the strong connection between chemostructural evolution and disk formation.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: An example of the observed spectrum from the spaxel in the galaxy center and Gaussian models of the observed emission lines. Panel (a): the color-composite image of galaxy ID 8365 is made from the JWST/NIRCam imaging (blue: F115W; green: F277W; red: F444W). The red box (﹩1\mathop{.}\limits^{^{\prime\prime} }8\times 3\mathop{.}\limits^{^{\prime\prime} }0﹩) represents the entire FoV of our slit-stepping 3D spectroscopy, and the white boxes mark the relative sizes of the five open microshutter slitlets. The observing strategy of the MSA-3D project acquires spectroscopy of our targets in 63 pointings in total, moving slitlets in nine steps of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩2 in the dispersion direction and seven dithers of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩075 in the cross-dispersion direction. For further details, refer to I. Barišić et al. (2024). Panel (b) shows the full observed spectrum from the spaxel in the galaxy center, indicated as a green box in panel (e), with the orange curves being the Gaussian-fitted emission line models. We detect pronounced nebular emission features in the galaxy center. We also zoom in on the line fitting results in panels (c) and (d). The gray vertical dashed lines represent the locations of Hβ, [O III], Hα, [N II], and [S II]. Panel (e): the flux map of the Hα emission line, where the ellipse represents the resolution element.
Paper: MSA-3D: Metallicity Gradients in Galaxies at z ∼ 1 with JWST/NIRSpec Slit-stepping Spectroscopy
Authors: Mengting Ju, Xin Wang, Tucker Jones, Ivana Barišić, Themiya Nanayakkara, Kevin Bundy, Claude-André Faucher-Giguère, Shuai Feng, Karl Glazebrook, Alaina Henry, Matthew A. Malkan, Danail Obreschkow, Namrata Roy, Ryan L. Sanders, Xunda Sun, Tommaso Treu, Qianqiao Zhou
Figure caption: The distribution of metallicity gradient slopes, in units of dex kpc−1. The black error bar shows the median 1σ uncertainty, highlighting the very small measurement uncertainties afforded by the high-quality MSA-3D data set. The metallicity gradients of our 25 galaxies are predominantly negative or flat, with slopes typically more positive than those of local spiral galaxies.
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Observational data fitted with ISEAge laboratory mixtures (solid lines), LIDA data (dashed, dotted and dashed–dotted gray lines), and simulated methane emission spectrum derived from TheoReTS data.
Paper: Solid and Gaseous Methane in IRAS 23385+6053 as Seen with Open JWST Data
Authors: Ruslan Nakibov, Varvara Karteyeva, Igor Petrashkevich, Maksim Ozhiganov, Mikhail Medvedev, Anton Vasyunin
Figure caption: Laboratory spectra data of pure N2O, N2O : H2O = 1 : 20, N2O : CO = 1 : 20, N2O : CO2 = 1 : 20. All the mixtures have the same column density of both N2O and a matrix molecule. The dashed lines mark the extreme peak positions of the N2O features.
Paper: The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion
Authors: Wafa Zakri, S. T. Megeath, William J. Fischer, Robert Gutermuth, Elise Furlan, Lee Hartmann, Nicole Karnath, Mayra Osorio, Emily Safron, Thomas Stanke, Amelia M. Stutz, John J. Tobin, Thomas S. Allen, Sam Federman, Nolan Habel, P. Manoj, Mayank Narang, Riwaj Pokhrel, Luisa Rebull, Patrick D. Sheehan, Dan M. Watson
Figure caption: Left: 4.5 μm light curves of HOPS 12 (top) and HOPS 124 (bottom). Included are the cryo observations from 2004, YSOVAR data from 2009–2010, OrionTFE measurements from 2016–2017, and Spitzer Beyond observations from 2019. HOPS 124 did not fall within the YSOVAR field. Dashed lines show the times of the MIPS, PACS, and FORCAST observations. Middle: Spitzer [3.6] − [4.5] colors of both protostars as a function of time. Right: Spitzer (4.5 μm), WISE, and NEOWISE (4.6 μm) light curves; these have been measured relative to the averaged Spitzer 2016–2017 magnitude (for Spitzer) or the averaged magnitude of the NEOWISE data bracketing the averaged date of the OrionTFE data (for WISE/NEOWISE). The Spitzer photometry for the 2004, 2010, and the 2016–2017 epochs have been averaged. The HOPS 12 points are for the combined East and West sources.
Paper: The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion
Authors: Wafa Zakri, S. T. Megeath, William J. Fischer, Robert Gutermuth, Elise Furlan, Lee Hartmann, Nicole Karnath, Mayra Osorio, Emily Safron, Thomas Stanke, Amelia M. Stutz, John J. Tobin, Thomas S. Allen, Sam Federman, Nolan Habel, P. Manoj, Mayank Narang, Riwaj Pokhrel, Luisa Rebull, Patrick D. Sheehan, Dan M. Watson
Figure caption: Spitzer 3.6 and 4.5 μm images of the HOPS 12 outburst (left, α = 83.°78584, δ = −5.°93174 J2000) and the HOPS 124 outburst (right, α = 84.°83327, δ = −7.°43644 J2000) with the locations of the protostars marked. The 2004 cyro images (top) show the protostars pre-outburst, while the OrionTFE images (bottom) show the protostars during the bursts.
Paper: The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion
Authors: Wafa Zakri, S. T. Megeath, William J. Fischer, Robert Gutermuth, Elise Furlan, Lee Hartmann, Nicole Karnath, Mayra Osorio, Emily Safron, Thomas Stanke, Amelia M. Stutz, John J. Tobin, Thomas S. Allen, Sam Federman, Nolan Habel, P. Manoj, Mayank Narang, Riwaj Pokhrel, Luisa Rebull, Patrick D. Sheehan, Dan M. Watson
Figure caption: The transmission profiles for the FORCAST 19.7 μm filter, FORCAST 25.3 μm filter, FORCAST 31.7 μm filter, and MIPS 24 μm filter. The IRS spectrum of HOPS 124 is also displayed. All have been normalized so that the peak value is unity.
Paper: The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion
Authors: Wafa Zakri, S. T. Megeath, William J. Fischer, Robert Gutermuth, Elise Furlan, Lee Hartmann, Nicole Karnath, Mayra Osorio, Emily Safron, Thomas Stanke, Amelia M. Stutz, John J. Tobin, Thomas S. Allen, Sam Federman, Nolan Habel, P. Manoj, Mayank Narang, Riwaj Pokhrel, Luisa Rebull, Patrick D. Sheehan, Dan M. Watson
Figure caption: Probability density functions (top) and cummulative probability distributions (bottom) for the burst interval. These are calculated for the entire cloud sample (left: 92 Class 0 protostars and 227 Class I/FS protostars), the YSOVAR field of the ONC (middle: 27 Class 0 protostars and 45 Class I/FS protostars), and all protostars in the clouds and in the ONC (right: 319 protostars in the clouds and 72 in the ONC). A 13 yr baseline is assumed. These are based on Equation (2) from Fischer et al. (2019) (also see Hillenbrand & Findeisen 2015; Contreras Peña et al. 2019).
Paper: The Rate, Amplitude, and Duration of Outbursts from Class 0 Protostars in Orion
Authors: Wafa Zakri, S. T. Megeath, William J. Fischer, Robert Gutermuth, Elise Furlan, Lee Hartmann, Nicole Karnath, Mayra Osorio, Emily Safron, Thomas Stanke, Amelia M. Stutz, John J. Tobin, Thomas S. Allen, Sam Federman, Nolan Habel, P. Manoj, Mayank Narang, Riwaj Pokhrel, Luisa Rebull, Patrick D. Sheehan, Dan M. Watson
Figure caption: Comparison of HOPS 383 and nearby protostars in the 70 μm Herschel/PACS image obtained on 2010 September 10 (left) and the 89 μm SOFIA/HAWC+ image obtained on 2019 September 10 (middle). The location of HOPS 383 is marked (α = 83.87421°, δ = −4.99754° J2000). Right: Light curve of HOPS 383 at 4.5 μm. The times of the MIPS, FORCAST, PACS, and HAWC+ observations are shown by the vertical lines.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: From top to bottom: shapes of the H2O, NH3, CO2 and H2S icelines (black dashed lines) at t = 50, 150, and 200 kyr of the CPD evolution. The hatched areas are located within the shadow cast by the CPD. We use the nominal model depicted in Section 3, with a metallicity 0.1 times protosolar. Iceline temperatures are determined using the equations of state compiled in A. Schneeberger et al. (2023).
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: Temperature and pressure profiles within the CPD after t = 50, 500, 1000, and 3000 kyr of evolution, using the accretion rate prescription from T. Sasaki et al. (2010), and a metallicity 0.1 times the protosolar one. The photosurface and the CPD’s scale height are represented by the white solid and dashed lines respectively. The hatched area is located within the shadow cast by the CPD.
Paper: Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure
Authors: Antoine Schneeberger, Olivier Mousis
Figure caption: CPD pressure profiles with α-viscosity parameters (from left to right columns) corresponding to 10−2, 10−3, and 10−4, depicted at t = 100, 150, and 200 kyr of the CPD evolution (from top to bottom rows). The solid white line represents the altitude of the photosurface. If the photosurface is not explicitly shown or represented in a given panel, it indicates its absence. The hatched areas are located within the shadow cast by the CPD.
Paper: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Brian Jackson, Lori Fenton, Travis Brown, Asier Munguira, German Martinez, Claire Newman, Daniel Viúdez-Moreiras, Matthew Golombek, Ralph Lorenz, Mark D. Paton, Dylan Conway
Figure caption: Telemetry streams from Ingenuity (panels (a) and (b)) and MEDA wind data (panel (c)) for flight 1. The legends provide the curve labels. Solid lines can be read off the left y-axis (as also indicated by the small arrows in the legend), while dashed lines can be read off the right y-axis. (Note that an azimuth of −180° is equivalent to +180°, and lines are not wrapped around in this figure to improve visibility.) In (a), the solid black line is Ingenuity’s altitude in meters; the pink line is dx/dt, which is the component of Ingenuity’s ground speed measured along the x-axis; the purple line is dy/dt, which is the component of Ingenuity’s ground speed measured along the y-axis; and the dashed green line is Ingenuity’s yaw in degrees. In (b), the solid orange line is the tilt angle t, and the dashed orange line is the tilt azimuth. In (c), the solid blue line is the wind speed measured by MEDA, and the dashed blue line is the wind azimuth measured by MEDA. The shaded gray region shows the time window during which we assumed the drone was in trimmed flight conditions (i.e., no net accelerations or torques), and it is during these periods that we estimated wind speeds.