adsabs/AstroCLIMB huggingface dataset:
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Atmospheric optical depth as a function of wavelength for fUV = 1 (purple curves) and fUV = 10 (red curves) Archean atmospheres. Different surface pressures, namely 4.0, 2.0, 1.0, and 0.5, are represented by tones gradually shifting toward lighter shades, indicating a transition from higher to lower pressure. Under 10 times stellar UV, the aerosol column thins (lower τ), consistent with nonmonotonic haze production in CO2-rich anoxic atmospheres where short-wavelength UV also enhances oxidative destruction of intermediates.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Biologically effective irradiance as a function of surface pressure based on results of Table 2. The Eff is calculated over a generation period for the two types of bacteria. The green area delineates the conditions where 10% of E. coli (left panel) and D. radiodurans (right panel) would thrive, whereas the white region represents an environment unsuitable for bacterial survival.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Action spectra, or biological response, for D. radiodurans (left) and E. coli (right).
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Top panel: Amplitudes of variability versus mass, color coded by variability type. The amplitude values are taken as medians across available sectors. Bottom panel: Timescales of variability are shown versus mass, sized by amplitude to the one-third power. Amplitude and timescale values are taken as medians across available sectors. The TESS 27 days sector duration is shown as a dashed horizontal line.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Q–M diagram for the portion of the HAeBes sample with more certain variable types, as shown by the color coding. Point size represents a scaling of variability amplitude to the one-third power. Data for objects with more than one sector of data appear as multiple points in this plot. The pile-up of points at Q = 1 illustrates the sequence of objects with no discernible period.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Top: Amplitudes for the sample of HAeBes presented in this work, as a function of timescale. Points are color coded by variability type and correspond to data from individual sectors; as such, some stars appear multiple times. Bottom: We show the sample quantities, but for the low-mass T Tauri stars from A. M. Cody & L. A. Hillenbrand (2018) and A. M. Cody et al. (2022).
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Spectral type distribution for the photometric sample employed in this work (HAeBes), as well as those from previous works on lower-mass stars (“CTTS”). Spectral types are labeled at the zero subtype (i.e., “A” is A0), and adopted from J. Guzmán-Díaz et al. (2021). If a range of spectral types is given, we take the subtype at the middle. As seen in the histogram, late B and early A stars comprise the most common types here, while earlier samples were dominated by late K and M types.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Same as Figure 7 for the modern Earth–like atmosphere model of TOI-700 d.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: H–R diagram for the sample, color coded by variability type. We display theoretical solar metallicity mass tracks (solid black curves) as well as a 2 Myr isochrone from C. T. Nguyen et al. (2022) and G. Costa et al. (2025). Spectral types are shown at the top, based on effective temperatures of stars in the HarchiBe sample. Point size represents a scaling of variability amplitude to the one-third power.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Light curves for two stars with pronounced changes in variability morphology and amplitude over a couple years. While relatively rare, these cases highlight the possibility that HAeBe variability drivers may shift dramatically on relatively short astronomical timescales.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Representative examples of light-curve morphology types from our Herbig Ae/Be sample observed by TESS. We omit eclipsing binaries and nonvariable objects.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: Abundance profiles for relevant isotopes that help identify the different parts of the CCSN ejecta (1H, 4He, 12C, 16O, and 28Si), 63Cu ejected and that includes the radiogenic contributions (63Cu*), are shown with respect to the mass coordinate (mass fraction X on the y-axis) for the models of MZAMS = 15 M⊙ at Z = 0.02 (left panel) and Z = 0.0001 (right panel). The relevant radiogenic parent species of 63Cu are also presented and plotted with dashed lines.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Keplerian orbital period of the inner dust disk versus variability timescale, scaled and color coded by variability type, as in Figure 8. Nonvariable objects and unknown types are excluded since they do not have a well-defined variability timescale. Eclipsing binaries are also omitted. The gray dotted–dashed line indicates the duration of a single TESS sector, while the dashed line indicates equality of the two timescales. We find that the vast majority of HAeBes variability observed here is dominated by timescales shorter than the inner disk orbital period.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Dereddened J − H versus H − Ks for our sources. The dashed quadrilateral region indicates the locus of HAeBes defined by J. Hernández et al. (2005). The corresponding locus for CTTS (M. R. Meyer et al. 1997) is shown as a solid line, while the sequence of dwarf stars from M. J. Pecaut & E. E. Mamajek (2013) is included as a dashed curve. A gray dashed vector marks the colors of an extincted B0 dwarf with various values of AV up to 16. All colors have been transformed to the 2MASS system.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 65Cu.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Accretion rate versus estimated inner disk dust radius, color coded by variability type, as in Figure 7. Point size scales with the amplitude of variability to the one-third power.
Paper: The Optical Photometric Variability of Herbig Ae/Be Stars from TESS
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Shreya Chandragiri, Marvin Morgan
Figure caption: Histogram of disk SED types, according to J. Guzmán-Díaz et al. (2021). In brief, the J/H/Ks label is an indication of the shortest wavelength at which an infrared excess appears. These types are broken down by variability class, as shown in the labels.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 67Zn.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The results of GCE calculations using pre-SN yields for the selected elements (Cu, Zn, Ga, and Ge) in comparison with observational data. The error bars in the red box show the typical observational uncertainties (σ; ±0.1 dex for x and ±0.2 dex in y). The uncertainties from the LO12 and OT20 rates are represented by the shaded regions (see text for details). The calculated results using the AD21, ND23, and CR18 rates are also presented. The crossing point of the dashed lines represents the solar metallicity ([X/Fe] = [Fe/H] = 0). The observational data are from C. Sneden et al. (1998), P. Bonifacio et al. (2009), R. G. Gratton et al. (2003), I. I. Ivans et al. (2003), B. E. Reddy et al. (2003, 2006), G. Bihain et al. (2004), R. Cayrel et al. (2004), T. Bensby et al. (2005), J. J. Cowan et al. (2005), D. K. Lai et al. (2008), A. Frebel et al. (2010), J. G. Cohen et al. (2013), M. N. Ishigaki et al. (2013), T. Bensby et al. (2014), I. U. Roederer et al. (2014), H. R. Jacobson et al. (2015), and V. M. Placco et al. (2015).
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The SFR, gas mass, inflow and outflow rates, and SN (CCSN and SN Ia) rates as a function of the galactic age are plotted for the OMEGA+ model. The observational constraints (from M. Kubryk et al. 2015) are plotted as the solid bars on the right side (t ≈ 13 Gyr).
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 70Ge.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: Evolution of the gas metallicity ([Fe/H], top; Z, bottom) predicted by the Milky Way model used in the present work. The vertical and horizontal dotted lines represent the time at which the Sun is assumed to form and the solar metallicity (M. Asplund et al. 2009), respectively. See B. Côté et al. (2019) for details as well.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: Post-SN stellar abundance profiles for major fuels (1H, 4He, 12C, 20Ne, 16O, 28Si, and 56Ni; upper panel), 65Cu (central panel), and 70Ge (lower panel) in the 15 M⊙ model at Z = 0.02.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: Sensitivity of GCE to varied resonance strengths (see Table 3). The top row is [Cu/Fe] and [Zn/Fe], and the bottom row is [Ga/Fe] and [Ge/Fe]. The results from each condition are normalized to the OT20 values. The magenta band shows the uncertainties derived from the OT20 rate.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 68Zn.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 74Ge.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 69Ga.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The post-SN results of GCE calculations for Cu, Zn, Ga, and Ge in comparison with observational data. The green bands show the pre-SN GCE variations using the upper limit by LO12 and the lower limit by OT20 and thus the possible maximum range from the current 22Ne+α reaction rate uncertainties. The pre-SN GCE using the CR18 rate is shown as well. The error bars in the red box show the typical observational uncertainties (σ; ±0.1 dex for x and ±0.2 dex for y). See Figure 11 for the observation data.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 64Zn.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 70Zn.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 71Ga.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 76Ge.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 72Ge.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 73Ge.
Paper: Impact of the Latest 22Ne+α Reaction Rates on Nucleosynthesis in Massive Stars and Galactic Chemical Evolution
Authors: Emma Kotar, Shuya Ota, Allyson Dewey, Joshua Millman, Lorenzo Roberti, Marco Pignatari
Figure caption: The same as Figure 1 but for 66Zn.
Paper: On the Distance to the Black Hole X-Ray Binary Swift J1727.8–1613
Authors: Benjamin J. Burridge, James C. A. Miller-Jones, Arash Bahramian, Steve R. Prabu, Reagan Streeter, Noel Castro Segura, Jesús M. Corral-Santana, Christian Knigge, Andrzej Zdziarski, Daniel Mata Sánchez, Evangelia Tremou, Francesco Carotenuto, Rob Fender, Payaswini Saikia
Figure caption: Estimates of E(B – V) for distances between 0 and 7.5 kpc along the line of sight to J1727. The 3D Galactic dust maps include Bayestar (blue line; G. M. Green et al. 2019) and Gaia (purple line; G. Edenhofer et al. 2024). We also use an update of the 2D “SFD” dust map (D. J. Schlegel et al. 1998) to remove extragalactic contamination that is referred to as the “corrected SFD” (CSFD; gray dashed line; Y.-K. Chiang 2023). To investigate the likely maximum E(B – V) values within this distance range, we use CSFD; as this only reports the total value for E(B – V) along the line of sight, it serves as a good estimate of the maximum E(B – V) in the direction of J1727 at high distances. From this, we derive a maximum E(B – V) ≈ 0.4. Despite each having significant caveats and the disagreement between Bayestar and Gaia in how gas is distributed along the line of sight, both appear to accumulate to roughly this maximum value. Lastly, our estimate of E(B – V) (pink dotted line) is derived from our near-UV observations. We use this estimate to conclude that values of E(B – V) ≫ 0.4 may not be reliable and suggest a distance to J1727 of ﹩5.{5}_{-1.1}^{+1.4}﹩ kpc with 1σ uncertainties, which are included for reference (orange dotted–dashed line and shaded region, respectively).
Paper: On the Distance to the Black Hole X-Ray Binary Swift J1727.8–1613
Authors: Benjamin J. Burridge, James C. A. Miller-Jones, Arash Bahramian, Steve R. Prabu, Reagan Streeter, Noel Castro Segura, Jesús M. Corral-Santana, Christian Knigge, Andrzej Zdziarski, Daniel Mata Sánchez, Evangelia Tremou, Francesco Carotenuto, Rob Fender, Payaswini Saikia
Figure caption: A consolidated view of the H I spectra for both the target, J1727 (red, left), and our reference source, J1733 (blue, right). We observed no significant (>3σ) absorption outside the velocities chosen as the x-axis range. The y-axis represents the H I absorption percentage. The dashed lines indicate the x- and y-axes’ origins. The vertical dotted lines indicate the maximum velocity at which significant absorption is observed. For J1727, these are 24.8 ± 2.8 and 18.7 ± 0.4 km s−1. For J1733, these are 30.4 ± 2.8 and 32.7 ± 0.4 km s−1. The top-left plot is the 32k-S spectrum for J1727 from 14 October 2023, while the bottom-left plot is the mean weighted J1727 spectrum achieved by combining both 32k-Z spectra from Figure 1. We generated the 32k-Z (32k-S) spectra for J1733 from observations on 6 September 2023 (14 October 2023) with the peak J1733 flux density measured to be 6.1 ± 0.1 Jy (6.0 ± 0.1 Jy), providing the significantly greater SNR compared to that of the J1727 observations.
Paper: On the Distance to the Black Hole X-Ray Binary Swift J1727.8–1613
Authors: Benjamin J. Burridge, James C. A. Miller-Jones, Arash Bahramian, Steve R. Prabu, Reagan Streeter, Noel Castro Segura, Jesús M. Corral-Santana, Christian Knigge, Andrzej Zdziarski, Daniel Mata Sánchez, Evangelia Tremou, Francesco Carotenuto, Rob Fender, Payaswini Saikia
Figure caption: Our H I absorption spectra along of the line of sight toward J1727. The top two plots are the 32k-S spectra, and the bottom two plots are the 32k-Z spectra, with LSR velocity bin widths that are 5.6 and 0.7 km s−1 wide, respectively. The dashed lines indicate the origins of the x- and y-axes. The y-axis represents the residuals after subtracting the continuum emission from the data, with 3σ uncertainties indicated by the shaded areas, both of which are presented as a percentage of the continuum flux density of the source. The vertical dotted lines indicate the maximum velocity taken as the midpoint of the bin at which significant (>3σ) absorption is observed. In chronological order, these maximum velocities are 19.2 ± 2.8, 6.1 ± 0.4, 24.8 ± 2.8, and 18.0 ± 0.4 km s−1. The significantly greater SNR of the 14 October 2023 spectrum meant we were able to observe significant (>3σ) H I absorption to greater velocities than observed in the 32k-Z spectra.
Paper: On the Distance to the Black Hole X-Ray Binary Swift J1727.8–1613
Authors: Benjamin J. Burridge, James C. A. Miller-Jones, Arash Bahramian, Steve R. Prabu, Reagan Streeter, Noel Castro Segura, Jesús M. Corral-Santana, Christian Knigge, Andrzej Zdziarski, Daniel Mata Sánchez, Evangelia Tremou, Francesco Carotenuto, Rob Fender, Payaswini Saikia
Figure caption: The distance posterior distribution produced from Monte Carlo calculations using the near-UV constraint on E(B – V). The solid vertical line represents the 0.5000 quantile, and the dashed vertical lines represent the 0.1585 and 0.8415 quantiles.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: On the Distance to the Black Hole X-Ray Binary Swift J1727.8–1613
Authors: Benjamin J. Burridge, James C. A. Miller-Jones, Arash Bahramian, Steve R. Prabu, Reagan Streeter, Noel Castro Segura, Jesús M. Corral-Santana, Christian Knigge, Andrzej Zdziarski, Daniel Mata Sánchez, Evangelia Tremou, Francesco Carotenuto, Rob Fender, Payaswini Saikia
Figure caption: The near-UV spectrum of J1727 as seen by HST/STIS (black), with a reddened power-law fit (green) to the data (Castro Segura et al. 2025, in preparation) The uncertainty around the fit is indicated as a shaded region. The vertical shaded regions were masked during the fit to avoid Fe and Mg lines that may influence the fit.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: The degree of heterogeneity indices of elements in representative samples based on μXRF results. The grayscale value (the range was set between 0 and 1) of each pixel represented its relative quantity of the corresponding element (Figures A2–A7). The variance of each subspectrum was used as an estimate of the degree of heterogeneity. Regardless of grain sizes, the variation of elemental concentrations represented by standard deviations of relative abundances of different elements ranged from ∼0.02 to 0.2 with a mean value of ∼0.1.
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: Distribution of major element contents in the samples of this database compared with other existing databases. (A) The distribution of oxide compositions in this library for MarSCoDe and the library for SuperCam (R. B. Anderson et al. 2022). (B) 3D principal component analysis of major oxide compositions of samples in this study, the expanded ChemCam calibration database (S. M. Clegg et al. 2017), the SuperCam calibration database (R. B. Anderson et al. 2022), and Mars data (A. T. Banin et al. 1992; S. R. Taylor & S. M. McLennan 2009; D. F. Blake et al. 2013).
Paper: An Inclusive Library for Quantitative Analysis of the Laser-induced Breakdown Spectra Acquired by the Zhurong Mars Rover
Authors: Shuai-Yi Qu, Jianxun Shen, Luning Li, Zhicheng Cui, Xuesen Xu, Ziyi Liu, Chengxiang Huang, Haohuan Li, Honglei Lin, Wei Lin, Yangting Lin
Figure caption: LIBS spectra of JMSS-1 acquired at different distances. (A) Comparison of LIBS spectra of JMSS-1 at 2, 2.3, 2.5, 3, 3.5, and 4 m, showing a negative correlation between peak intensity and distance, the representative characteristic peaks of major elements are indicated at the corresponding positions in the figure. (B) Variations in characteristic peaks of selected elements in JMSS-1 at different distances. Different elements exhibit distinct trends with increasing distance, illustrating the complexity of the distance effect on LIBS spectra.