adsabs/AstroCLIMB huggingface dataset:
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as Xe-types. Plotted are (64) Angelina (DeMeo et al. 2009), CR2 chondrite EET 92042 (<125 μm; red line), CM2 chondrite LEW 88001 (<125 μm; blue line), and H6 chondrite Ozona (<50 μm; green line). The Angelina spectrum was normalized to unity at 0.55 μm and then multiplied by 0.474 (Shevchenko & Tedesco 2006). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as Xc-types. Plotted are (21) Lutetia (DeMeo et al. 2009; black open squares), EH3 chondrite KLE 98300 (<45 μm; red line), CM2 chondrite Dhofar 735 (<125 μm; blue line), and L5 chondrite Wittekrantz (25–250 μm, dark fraction; green line). The Lutetia spectrum was normalized to unity at 0.55 μm and then multiplied by 0.2212 (Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as S-types. Plotted are (7) Iris (DeMeo et al. 2009; black open squares), L5 chondrite Blackwell (<150 μm; red line), H6 chondrite Ozona (<150 μm; blue line), and acapulcoite Dhofar 125 (<125 μm, treated with ethanolamine thioglycolate to remove terrestrial weathering; green line). The Iris spectrum was normalized to unity at 0.55 μm and then multiplied by 0.2766 (IRAS albedo; Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as Sr-types. Plotted are (237) Coelistina (black open squares; DeMeo et al. 2009), L4 chondrite Rio Negro (<150 μm, metal removed; red line), H4 chondrite Chela (<150 μm, metal removed; blue line), and howardite PCA 02015 (<40 μm; green line). The Coelistina spectrum was normalized to unity at 0.55 μm and then multiplied by 0.2108 (IRAS albedo; Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as L-types. Plotted are (387) Aquitania (DeMeo et al. 2009; open black squares), EL4 chondrite MAC02747 (<45 μm; red line), CI1 chondrite (Orgueil) (<35 μm; blue line), and CM2 chondrite A-881280 (<125 μm; green line). The Aquitania spectrum was normalized to unity at 0.55 μm and then multiplied by 0.1900 (Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as Q-types. Plotted are (1862) Apollo (DeMeo et al. 2009; black open squares), L6 chondrite Harleton (125–500 μm; red line), LL5 chondrite Chelyabinsk (<125 μm; blue line), and H6 chondrite Kernouve (<125 μm; green line). The Apollo spectrum was normalized to unity at 0.55 μm and then multiplied by 0.20 (Rozitis et al. 2013). The error bars for the asteroid spectrum are 1σ.
Paper: Surface Properties of the Kalliope–Linus System from ALMA and VLA Data
Authors: Katherine de Kleer, Saverio Cambioni, Bryan Butler, Michael Shepard
Figure caption: Disk-integrated brightness temperature spectrum of Kalliope. All flux densities have been corrected to an asteroid–Sun distance of 2.9112 au (Kalliope’s semimajor axis a) using ﹩\sqrt{d/a}﹩ where d was the separation in astronomical units at the time of the measurement. The conversion to T  b  is calculated using the Planck function, and assumes an effective radius of 75 km. The model surface temperatures for the ALMA and VLA data are calculated for Γ = 116, and differ because Kalliope’s equator is facing the Sun at the time of the ALMA data set, while the pole is facing the Sun at the time of the VLA data set. These lines also therefore represent upper and lower bounds on the surface temperature at other orientations. South Pole Telescope (SPT) data are from P. M. Chichura et al. (2022) and Atacama Cosmology Telescope (ACT) data from J. Orlowski-Scherer et al. (2024), and have been converted from flux density to brightness temperature in the same way as the ALMA and VLA data; these data are aggregated over tens to hundreds of individual measurements that are frequently at the <1σ level.
Paper: Surface Properties of the Kalliope–Linus System from ALMA and VLA Data
Authors: Katherine de Kleer, Saverio Cambioni, Bryan Butler, Michael Shepard
Figure caption: Millimeter–centimeter spectra of asteroids that have been observed at high spatial resolution and for which emissivities have been calculated from thermophysical models. Millimeter data for (21) Lutetia and (2867) Šteins are from the MIRO instrument on the Rosetta spacecraft (S. Gulkis et al. 2010, 2012); 1.3 mm data on (16) Psyche are from K. de Kleer et al. (2021b); radar data are from C. Magri et al. (2007) and M. K. Shepard et al. (2015, 2021), and Kalliope’s radar albedo has been corrected to its updated diameter. Asteroids are designated by spectral type in the Tholen and Bus–DeMeo classification schemes (D. J. Tholen 1984; S. J. Bus 1999; F. E. DeMeo et al. 2009).
Paper: Surface Properties of the Kalliope–Linus System from ALMA and VLA Data
Authors: Katherine de Kleer, Saverio Cambioni, Bryan Butler, Michael Shepard
Figure caption: Simple thermophysical models for an equatorial point on a spherical asteroid with the rotation periods of Kalliope (4.148 hr) and Linus (3.596 days), demonstrating the change to the diurnal thermal emission curve due to rotation rate alone. (a) Temperature of the surface; (b) ratio of thermal emission from the surface per unit area; (c) thermal emission integrated through the subsurface assuming δ elec = 10λ and converted to brightness temperature; (d) ratio of thermal emission per unit area including the subsurface emission. Note that because (c) and (d) account for subsurface emission, they also capture the effect of the rotation period on the thermal diurnal skin depth.
Paper: Surface Properties of the Kalliope–Linus System from ALMA and VLA Data
Authors: Katherine de Kleer, Saverio Cambioni, Bryan Butler, Michael Shepard
Figure caption: Flux density per unit area for Kalliope compared to Linus. Top: the projected surface area ratio of Kalliope to Linus at the time of each ALMA image. Middle: the flux density ratio of Kalliope to Linus. Bottom: the ratio of flux density per unit area of Kalliope to Linus. The uncertainties on the area ratio are set by the uncertainties on Linus’ diameter alone (and therefore do not represent statistical scatter between points but rather a systematic uncertainty that is the same across all points). The uncertainties on the flux density are propagated from the measurement uncertainties on both quantities and are statistical scatter. The final stated value of 0.87 ± 0.05 has an uncertainty that is the sum in quadrature of the uncertainties on the mean of the flux density ratio and the uncertainty on Linus’ area.
Paper: Surface Properties of the Kalliope–Linus System from ALMA and VLA Data
Authors: Katherine de Kleer, Saverio Cambioni, Bryan Butler, Michael Shepard
Figure caption: Results from the local model. (a) Time-average of the data minus the model. (b) Goodness of fit of the local thermophysical model of Kalliope for the ALMA data. (c) Best-fit Γ. (d) Uncertainty in Γ. (e) Best-fit dielectric constant, ϵ. (f) Uncertainty in ϵ.
Paper: ASKAP-EMU Discovery of “Raspberry”: A New Galactic SNR Candidate G308.73+1.38
Authors: Sanja Lazarević, Miroslav D. Filipović, Bärbel S. Koribalski, Zachary J. Smeaton, Andrew M. Hopkins, Rami Z. E. Alsaberi, Velibor Velović, Brianna D. Ball, Roland Kothes, Denis Leahy, Adriano Ingallinera
Figure caption: RGB composite image where the total intensity map of Raspberry, observed by ASKAP at ν = 944 MHz, is in red and blue while WISE 12 μm infrared image is in green. To present the structure of Raspberry, we used different colormaps and adjusted contrast levels. A linear scale is applied to all images. The inset is the ASKAP Stokes-V zoomed-in image showing the possible progenitor source.
Paper: The Hg II Line at 5677.10 Å: A New Proxy to Derive Abundances of Mercury in Late B-type Stars?
Authors: Richard Monier
Figure caption: Left: Line synthesis of the Hg II line at 5677.10 Å of κ Cnc (observed spectrum in black, synthetic spectrum in red, 53 Tau in green), Right: Same comparison for HD 58661.
Paper: Ultracool Dwarf Absolute Magnitude Versus Spectral Type Relations for Euclid and Roman Near-infrared Filters
Authors: Aniket Sanghi, Michael C. Liu, Trent J. Dupuy, William M. Best, Robert J. Siverd, Zhoujian Zhang
Figure caption: Absolute magnitudes derived for our sample of 1054 ultracool dwarfs as a function of their spectral type (SpT) in various Euclid and Roman filters (AB magnitude system). Field objects, low gravity objects, and young moving group members are marked by gray, cyan, and blue points respectively. Random scatter in the x-direction with amplitude 0.35 SpT is applied to avoid overlapping points. Due to the large number of points, uncertainties in individual measurements are not shown. The median uncertainty in absolute magnitude is 0.045 mag. The black solid and dashed lines are the best-fit polynomial relations for the field and young objects, respectively. The shaded blue and orange regions represent the rms scatter about the field and young object fits, respectively.
Paper: Progenitor Stars Calculated with Small Reaction Networks should not be Used as Initial Conditions for Core Collapse
Authors: M. Renzo, J. A. Goldberg, A. Grichener, O. Gottlieb, M. Cantiello
Figure caption: Comparison of chemically homogeneous models at the onset of core-collapse. Right: HRD (one dot every 105 yr). Top left: density. Middle left: Y  e , relative difference in red (right vertical axis). Bottom left: specific angular momentum j. The dashed line shows j ISCO assuming the accretion of the enclosed m and j. Dots correspond to regions that collapse forming a disk, j ≥ j ISCO.
Paper: Recovery and Classification of Spherules from the Pacific Ocean Site of the CNEOS 2014 January 8 (IM1) Bolide
Authors: A. Loeb, T. Adamson, S. Bergstrom, R. Cloete, S. Cohen, Kevin Conrad, Laura Domine, H. Fu, C. Hoskinson, E. Hyung, S. B. Jacobsen, M. Kelly, J. Kohn, E. Lard, F. Laukien, J. Lem, R. McCallum, R. Millsap, C. Parendo, M. I. Pataev, C. Peddeti, J. Pugh, S. Samuha, D. D. Sasselov, M. Schlereth, J. Siler, A. Siraj, P. M. Smith, R. Tagle, J. Taylor, R. Weed, A. Wright, J. Wynn
Figure caption: Panel (a): Atomic Mg–Si–Fe plot of microXRF data for 745 IM1 site spherules. The spherule groups are compared to reference values of Earth materials (Bulk Earth, bulk silicate Earth (BSE), upper continental crust (UCC), shale, normal midocean ridge basalts (N-MORB), Hawaiian basalt (BHVO-1), Columbia River basalt (BCR-1), Guano Valley andesite (AGV-1) and CI meteorites. Panel (b): Typical BeLaU abundance pattern of a spherule in our sample (S21). Panel (c): Comparison BeLaU with the NIST coal fly ash standard SRM1633a for 55 elements.
Paper: TOI-6883.01: A Single-transit Planet Candidate Detected from TESS
Authors: G. Conzo, M. Moriconi
Figure caption: LATTE-Report (Eisner 2022) results: (a) Transit light curve in the BJD time-domain and normalized flux; (b) Background light curve in the BJD time-domain and normalized flux; (c) Centroid light curve in the BJD time-domain and x-position; (d) Centroid light curve in the BJD time-domain and y-position; (e) Grid of pixels with target pixel illumination and event display; (f) Comparison of pixels illuminated by the target before and during transit.
Paper: Activity Discovered on Mars-Crossing Jupiter Family Comet 2018 OR by Citizen Scientists
Authors: Kennedy A. Farrell, Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Jarod A. DeSpain, Mark Jesus Mendoza Magbanua, Nima Sedaghat, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes
Figure caption: 2018 OR (at center) with a tail in the anti-velocity (red-outlined black arrow) and anti-solar (yellow arrow) directions in 126″ × 126″ images. (a) UT 2018 September 5, 160 s GRI-band MegaPrime imager on the 3.6 m CFHT (proposal 18BH09, PI Wainscoat). (b) UT 2018 September 6, 46 s r-band DECam (Prop. ID 2014B-0404, PI Schlegel, observer Z. Slepian). (c) UT 2018 September 17, 30 s r-band ZTF camera (48″ Samuel Oschin telescope, Palomar).
Paper: Gnuastro: Measuring Radial Profiles from Images
Authors: Raúl Infante-Sainz, Mohammad Akhlaghi, Sepideh Eskandarlou
Figure caption: Color image and surface brightness radial profiles of M81 galaxy. Left: Color image with gray background obtained by using the astscript-color-faint-gray script (Infante-Sainz & Akhlaghi 2024). Right: Surface brightness radial profiles of the rSDSS image, measured with two different operators. The y-axis represents the surface brightness (SB), while the x-axis represents the distance to the center of the galaxy. The red circles correspond to the measurements obtained by a simple mean, and they exhibit peaks due to the bright objects (stars). In contrast, the blue squares represent the measurements obtained using a 3σ clipped mean, resulting in a smoother profile by removing the extreme outlier values (for example those from contaminant sources).
Paper: A Bigger Cloud 9? New H I Observations of the RELHIC Candidate M94- Cloud 9
Authors: Ananthan Karunakaran, Kristine Spekkens
Figure caption: GBT H I spectrum of M94-CL9 shown in blue and the FAST spectrum from Z23 shown in gray. The velocity range of the H I emission noted by Z23 is shown with the vertical dashed lines. We highlight the difference in H I emission as the hatched and shaded regions.
Paper: Probing Shocked Ejecta in SN 1987A with XRISM-Resolve: The Effects of the Gate Valve Closed
Authors: Vincenzo Sapienza, Marco Miceli, Aya Bamba, Salvatore Orlando, Shiu-Hang Lee, Shigehiro Nagataki, Masaomi Ono, Satoru Katsuda, Koji Mori, Makoto Sawada, Yukikatsu Terada, Roberta Giuffrida, Fabrizio Bocchino
Figure caption: Upper panel: Synthetic XRISM-Resolve spectrum of SN 1987A for the year 2024 (assuming the gate valve closed) with an exposure time of 160 ks including bulk motion Doppler broadening and binned using the J. S. Kaastra & J. A. M. Bleeker (2016) optimal binning algorithm. The synthetic XRISM-Resolve spectral model is superimposed with a black dashed line. The red curve shows the contribution of the CSM (ER and H II) to the spectral model, while the blue curve shows the contribution of the ejecta. Lower left panel: Close-up view of the spectrum shown in upper panel in the 2.38–2.65 keV band with best-fit model and residuals. Lower right panel: Close-up view of the spectral model shown in upper panel in the 2.38–2.65 keV band.
Paper: An Independent Discovery of the 1946 Eruption of the Recurrent Nova T Coronae Borealis and an Early Prediction of a Future Outburst
Authors: J. H. Shears
Figure caption: Letter from N.F.H. Knight to VSS Director W.M. Lindley on February 10 (first page).
Paper: A Comment on the Solar Activity Level in 1791 by Lorenzo Hervás y Panduro
Authors: A. J. P. Aparicio, J. M. Vaquero
Figure caption: Frontispiece of the book entitled “Static journey to the planetary world” (1793) (left) and page 157 containing an interesting comment on solar activity in 1791 (right).
Paper: Gnuastro: Generating Polar Plots in Astronomical Images
Authors: Sepideh Eskandarlou, Mohammad Akhlaghi
Figure caption: Construction of polar plots. The top row, shows the radial map, input image (M101 as imaged in J-PLUS) and azimuthal map (from left to right). In radial and azimuthal maps, the color changes from dark blue to yellow as the angle and radius become larger. The combination of the azimuthal angle, input image, and radial profile generates the polar plot displayed in the bottom row. The horizontal represents the angles derived from the azimuthal data. As a demonstration, the dark purple and blue lines in the top-middle panel show the pixels at a constant azimuthal angle of 45° and 135° respectively. The vertical axis represents the radii derived from the radial profile, and the value of each pixel corresponds to the value of the input image’s pixels. As a demonstration, the green and yellow circles in the top-middle panel show the pixels at a constant radius of 112 and 135 respectively.
Paper: Kinematic Association of Two FU Orionis Stars with Young Clusters in Orion
Authors: Tamojeet Roychowdhury, Lynne A. Hillenbrand
Figure caption: Top panels: Gaussian-smoothed histograms (see text) of ﹩{\mu }_{\alpha }^{* }﹩, μ  δ  and RV for the λ Ori cluster, along with the best-fit Gaussian model of the peak. Sub-samples include the full set, the proper-motion (2D) comovers, and the 3D comovers. Values for FU Ori are marked, and their n − σ differences indicated. Sky positions of these 2D and 3D comovers that satisfy the restriction of velocity difference ≤3σ  v  are shown, where expressions and obtained values of σ  v  are given in the text. Numbers in brackets show the number of comovers out of the total number of stars satisfying the error/quality cuts in the ±25 pc region. Bottom panels: Similar histograms and sky positions for the Orion Nebula cluster stars, V883 Ori, and its 2D and 3D comovers.
Paper: Predicting CO2 Gas Layer Thickness due to Mantle Outgassing in the Exoplanet Census
Authors: Eva Stafne, Juliette Becker
Figure caption: Exoplanet gas layer thickness as a function of semimajor axis and atmospheric temperature using equations from Dorn et al. (2018), Weiss & Marcy (2014), and a mask derived from Lopez et al. (2012). Each point represents an exoplanet <5M ⊕ and the point colors denote the expected gas layer thickness of CO2. Data was obtained from the NASA/Caltech Exoplanet Archive. The shaded area represents the location of the habitable zone, defined as the region with planetary effective temperatures between 273 and 373 K.
Paper: Ellipse-fitting in Mock Images of TNG50 Barred Galaxies
Authors: Gustavo F. Gonçalves, Rubens E. G. Machado
Figure caption: Method for estimating bar properties via ellipse fitting in a simulated barred galaxy. The left column displays the data and noise-free analysis, while the right column shows the data after applying synthetic noise and PSF. The top panels present the mock image based on mass distribution. The middle panels show the ellipses generated through ellipse fitting. The lower panels illustrate the ellipticity of the fitted ellipses as a function of the semimajor axis, where the dashed line indicates the obtained bar length. The barred galaxy in this example is subhalo ID394621 at z = 0, shown face-on.
Paper: A Two-month Mini-moon: 2024 PT5 Captured by Earth from September to November
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: Evolution of the relative mean longitude of 2024 PT5 and its geocentric energy (top), and its relative semimajor axis as a function of its relative mean longitude and its nominal geocentric motion (bottom, Earth in blue, captures in red). The top-right and bottom panels focus on the time interval (−1,  1) yr. The bottom-left panel shows the evolution around the mini-moon episode. Top panels show the evolution of the nominal orbit (in black) and those of control orbits with state vectors separated ±3σ (light-green/green) and ±9σ (light-/dark-red) from the nominal one. The unit of energy is such that the unit of mass is 1 M ⊙, the unit of distance is 1 au, and the unit of time is one sidereal year divided by 2π. The output interval is 0.36525 day. The origin of time is epoch 2460600.5 (2024 October 17.0) TDB.
Paper: Spectral Index Asymmetries in Double Radio Sources from the VLA Sky Survey
Authors: Rachael Howard, Mark Lacy
Figure caption: A comparison of the difference spectral index and ratio of lobe length for the full data set, using the spectral indices and flux weighted spectral indices. Both graphs show a slight, though statistically insignificant positive correlation.
Paper: Sensitivity of Global Oscillation Frequencies to Solar Activity on Short Timescales
Authors: Sushanta C. Tripathy, Kiran Jain
Figure caption: (a) Temporal variation of mean frequency shifts (symbols) and their smoothed variation over 1 yr period (solid line) for 9 days (blue) and 108 days (green) time series. The vertical dashed lines demarcate the three solar cycles. For clarity, the errors are shown only for a few data points. The solid red line illustrates the variation in radio flux calculated over 9 days intervals. (b) The solid lines indicate linear fits between the frequency shifts and 10.7 cm radio flux; blue for 9 days and green for 108 days data sets. The open and filled symbols represent cycles 23 and 24, respectively. Errors in fittings are shown in the right bottom corner.
Paper: Finding Passive Galaxies in H I-MaNGA: The Impact of Star Formation Rate Indicator
Authors: Nora Salem, Karen L. Masters, David V. Stark, Anubhav Sharma
Figure caption: (a): Scatter plot of Hα-, SSP-, and UV-derived sSFRs against W2 − W3 (IR) for H I-rich MaNGA galaxies (colors as in the legend in panel (b)). Overplotted are lines of binned averages. The solid vertical line shows W2 − W3 = 2, and the horizontal lines shows sSFR = 10−11.15 (solid) or 10−10.4 (dashed). (b): Histograms of stellar masses for all H I-rich low-SF samples. (c/d): As (b) for H I mass fraction and Hα velocity dispersion.
Paper: Variability Census of Legacy Catalogs. III. 8600+ New δ Scuti and γ Doradus Stars 
Authors: Ai-Ying Zhou
Figure caption: Example TESS light curves of 20 newly identified γ Dor pulsating variables. These plots were generated during automated batch processing.
Paper: Multi-color Photometry of Near-Earth Asteroid (415029) 2011 UL21
Authors: Bojan Novaković
Figure caption:  BVR photometry observations of 2011 UL21. The upper plot displays the measured apparent magnitudes in the B-band (black circles), V-band (gray squares), and R-band (black asterisks). The lower panel presents the asteroid's color indices, B − V and V − R. Red crosses indicate the nominal values for 2011 UL21 and their associated 1σ uncertainties, obtained in this work and by T. Hromakina et al. (2021). For reference, the typical color indices for different taxonomic classes from C. L. Dandy et al. (2003) are also shown (black circles).
Paper: Sizes and Stellar Masses of the Little Red Dots Imply Immense Stellar Densities
Authors: Carl Audric Guia, Fabio Pacucci, Dale D. Kocevski
Figure caption: Statistical descriptors of the population of LRDs presented in H. B. Akins et al. (2024) and D. D. Kocevski et al. (2024). Left: distribution of the inferred core stellar densities. Right: combined distribution of effective radii and densities.
Paper: Database of Candidate Targets for the LIFE Mission
Authors: Franziska Menti, José A. Caballero, Mark C. Wyatt, Antonio García Muñoz, Keivan G. Stassun, Eleonora Alei, Markus Demleitner, Grant Kennedy, Tim Lichtenberg, Uwe Schmitt, Jessica S. Schonhut-Stasik, Haiyang S. Wang, Sascha P. Quanz
Figure caption: Spectral distribution of stars in the LIFE target database (dark blue), LIFE-StarCat (light blue), HPIC (green), and SPORES (olive).