adsabs/AstroCLIMB huggingface dataset:
Paper: Revisiting Seager’s 2013 Habitability Diagram with 2025 Data
Authors: Christina X. Liu, Jonathan H. Jiang
Figure caption: Top: single-host star mass vs. exoplanet orbital semimajor axis diagram. Exoplanets are colored by type and scaled by radius. Each pair of red and blue markers show the computed inner and outer HZ boundaries respectively for each host star, with the 5th-degree polynomial fits (from the least squares regression) indicated by the red and blue solid curves. Graphs on the mid-left, mid-right, bottom-left, and bottom-right are the breakdown diagrams for Terrestrial, Super-Earth, Neptune-Like, and Gas-Giant exoplanets respectively.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XX. HD 77350
Authors: Richard Monier
Figure caption: Left: synthesis of the 4475–4500 Å spectral interval (observed spectrum in black, synthetic spectrum in red), Right: the Hg II line at 5677.10 Å is not detected in the ELODIE spectrum of HD 77350.
Paper: Disentangling Joint Light Curves Using Photocenter Shifts: A Case Study Using NEOWISE Data
Authors: Bringfried Stecklum
Figure caption: Left: RGB composites (field of view 20″ × 20″) based on images from ALLWISE (top) and IRAC (bottom). SPICY 1474 is marked by the red circle. Center: Centroid positions relative to that resulting from GAIA DR2 positions and IRAC I1 fluxes (diamond symbol). The cross marks the SPICY 1474 position while that of SPICY 1478 is outside the field. (NEO)WISE epochs are color-coded. Right: NEOWISE light curves: blue—W1, red—W2; dashed line—SPICY 1474, light dashed line—SPICY 1478, full line—joint. The unTimely values have filled symbols (asterisks—SPICY 1474, squares—SPICY 1478). The unTimely W2 light curve of SPICY 1478 is marked by black-bordered symbols since it deviates from the disentangled one.
Paper: Swift-XRT Observations and Upper Limits at Five LHAASO Galactic Sources
Authors: Amiri Walker, Ella Werre, Shaan Karim, Stephen DiKerby
Figure caption: Swift-XRT exposures for J1928 (left) and J1959 (right), showing the detected X-ray source (green circle) and optical loading detections (red dash circles), along with the LHAASO uncertainty ellipse for J1959 (white dashed).
Paper: Gaia’s Faintest Stars
Authors: Jeremy Mould
Figure caption: (a) HR diagram for the sample. Stars in red have Gaia radial velocities. Brown dwarfs have been added (blue open circles, the UCD sample). The red lines are Atmos2020 models (M. Phillips et al. 2020) with ages exceeding 0.5 Gyr and masses near 0.05 M⊙; the branch labeled 0.019 is 0.019 M⊙, and the dashed red line is a temperature sequence at 0.1 Jupiter radius (RJ). A model for Jupiter mass and age 1 Myr is at G = 32 and Bp − Rp = 4. The lower extension to the figure shows the predicted G magnitudes of m8 to m11 PBH, m10 being the optically brightest. (b) Tangential velocities of the sample (black). Stars fainter than G = 17 mag (solid green). UCD stars from Sarro et al. (2022, blue). In spite of RPM selection these are disk kinematics. (c) The histogram is the mass distribution of solar system planets. The number of microlensing planet mass objects per host star is shown for M stars in red and G stars in green (D. Suzuki et al. 2016). The blue dashed lines bound the distribution of Free Floating Planets (FFPs) claimed by T. Sumi et al. (2023). The purple dotted line is a theoretical FFP distribution by G. Coleman & W. Derocco (2025).
Paper: On the Prevalence of Early Mass Transfer for Very Massive Binaries
Authors: C. A. Burt, M. Renzo, A. Grichener, N. Shah
Figure caption: Each panel contains 15 stellar MESA models spanning from 30 M⊙ star (longer lifetimes) to 100 M⊙ (shorter lifetimes). The top panels show models with I. Brott et al. (2011)-like “large” overshooting (A. Claret & G. Torres 2018), the middle panels show models without overshooting, and the bottom panels plot models generated using COMPAS based on analytic fits to stellar models from O. R. Pols et al. (1998). The left (right) panels have metallicity Z = 0.001 (Z = 0.0001). Dashed red (blue) lines mark the maximum radius during the main sequence (during the model’s runtime). The red (blue) shaded areas correspond to case A (case B) mass transfer.
Paper: Comparative Analysis of Polarization in Interstellar Comet 3I/ATLAS with Distant Solar System Comets
Authors: Evgenij Zubko, Gorden Videen
Figure caption: Degree of linear polarization as a function of phase angle measured in the R filter for 7 distant comets and for the interstellar Comet 3I/ATLAS (Z. Gray et al. 2025).
Paper: The Late Infrared Spectrum of the Very Slow Nova V5558 Sagittarii
Authors: Richard J. Rudy, Ray W. Russell, Michael L. Sitko
Figure caption: Infrared spectrum of the nova V5558 Sgr from 2346 days after discovery and 2260 days after maximum visible brightness. The spectrum is that of a moderately high excitation nova displaying a number of coronal lines (defined here as collisionally excited forbidden lines whose parent ions require ≥ 100 eV to form) labeled in blue. Other evidence of high excitation includes the prominence of the He II spectrum, with some very weak lines being detectable (e.g., the He II 8–13 transition at 2.3470 μm). Lines with unknown identifications are preceded by a question mark; lines with uncertain identifications or detections have a following question mark. With the exception of the line at 1.3375 μm, all of the infrared [Fe VI] features (labeled in red) are well detected.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXV. HD 32964 B (66 Eri B)
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 3983.93 Å of 66 Eri B (observed spectrum in black, synthetic spectrum in red), Right: synthesis of four Fe II lines of 66 Eri B from 4500 to 4540 Å.
Paper: Refining the Migrating Differentiated Planetesimal Disruption Model for Classical T-Tauri Star RW Aur A’s Dimming Events
Authors: C. M. Lisse, M. L. Sitko, S. J. Wolk, H. M. Günther, S. Brittain, T. Beck, C. Chen, B. Sargent, J. D. Green, J. Steckloff, B. C. Johnson, C. C. Espaillat, M. Koutoulaki, A. P. Jackson, T. Mittal, S. Silverberg
Figure caption: (a): Four near-infrared lines of Fe II from the RWAurA spectra of Note1 (Figure 1(a)), with the nominal Fe II emission line wavelength denoted by the vertical dashed line. Unlike the majority of the observed emission lines from the system, all show bifurcated red/blue shifted structure due to high velocity jet outflow, and decreasing amplitude with time since the first observation in fall 2018, 4 yr into the 2014–2020 event. (After C. M. Lisse et al. 2022) (b): 0.96–1.06 um IRTF/SpeX spectrum of RW Aur A from C. M. Lisse et al. (2022), re-analyzed by comparison to a hot novae source with gas temperatures better matching the ∼20,000 K of RW Aur A’s jets, and allowing identification of strongly bifurcated lines of S I, S II, and N I. (c): Imagery of the RW Aur A red jet in the light of Fe II 1.644 um, showing a new clump of material leaving the inner system in 2014. After M. Takami et al. (2020). (d): Spectral X-ray monitoring of RW Aur A using Chandra, showing the normal emission seen for the system in 2013 (red), the total extinction of soft X-ray emission in 2015 (purple), and the gradual clearing and emergence of a hard 6.6 keV Fe X-ray line (black). After H. M. Günther et al. (2018). (e): 0.7–35 um quiescent state SED of the RW Aur A+B system created by concatenating 2007 era IRTF/SpeX and Spitzer/IRS spectra. Blackbody elements at 4000 K (photosphere), 1300 K (inner accretion disk wall), and 190 K (accretion disk gap) are identified. After C. M. Lisse et al. (2025). (f): Emissivity spectrum created by removing the blackbody elements from (e), and matching them to the best-fit linear sum of a library of 100+ astrominerals. Common materials like olivines and pyroxenes are found, but so too are silica and alumina, products of high temperature/low pressure rocky material alteration.
Paper: Real-time Early Solar System Evolution in RW Auriga A: A New Major Dimming Event has Started in 2025 February
Authors: C. M. Lisse, M. L. Sitko, S. J. Wolk, H. M. Günther, S. Brittain, T. Beck, C. Chen, B. Sargent, J. D. Green, J. Steckloff, B. C. Johnson, C. C. Espaillat, M. Koutoulaki, A. P. Jackson, T. Mittal, S. Silverberg
Figure caption: (a): Comparative near-infrared spectroscopy of the RW Aur A and B systems. After C. M. Lisse et al. (2022). (b): ALMA structure of the RW Aur A+B system. After Rodriguez et al. (2018). (c): Close-up ALMA imagery of the RW Aur A and B disks. After Kurtovic et al. (2024). (d): AAVSO RW Aur A Optical Lightcurve, 2005–2025 (B. K. Kloppenborg 2025). Inset: −0.012 mag day−1 ingress lines fit to 4 of the observed downturns. (e): RW Aur A has marked, clumpy, fast moving (100–200 km s−1) jets detected in S II (C. Dougados et al. 2000) and Fe II (M. Takami et al. 2020, Note2). No such structures are associated with “normal” RW Aur B.
Paper: A New Velocity-dispersion Profile for the Core of 47Tuc
Authors: Alexander Petroski, Dana I. Casetti-Dinescu, Terrence M. Girard, Roberto Baena-Gallé
Figure caption: (Top) Proper-motion dispersion in the radial direction. (Middle) Proper-motion dispersion in the tangential direction. (Bottom) Anisotropy profile of the cluster. In all three plots, our new data are plotted in blue, and the data obtained by M. Libralato et al. (2022) are plotted in gold with red error bars.
Paper: Discovery of a New Satellite or Ring Arc around (50000) Quaoar
Authors: Richard Nolthenius, Kirk Bender, Daniel V. Cotton, Benjamin C. N. Proudfoot, John Irwin
Figure caption: (a) 0.91 m full light curve, (b) 0.91 m occultation profile, consistent with a square wave drop to zero, (c) 0.36 m light curve showing occultation profile and timing details, (d) Sky plane geometry of the MIRA occultation relative to known structures, (e) JWST light curve (B. Proudfoot et al. 2025) shows no opacity (green regions) from a putative 3rd ring aligned with our MIRA occultation.
Paper: Unveiling the Dynamics of Supernova: A Use of Dynamic Mode Decomposition
Authors: Ribhu Pal, Arnab Roy, Abanti Datta
Figure caption: (a) ﹩{\mathrm{log}}\,(\rho )﹩ distribution, and (b) filaments formation at t = 8.0, and (c) Eigenvalues plot.
Paper: Morphologies of Changing Look Active Galactic Nuclei Host Galaxies in Galaxy Zoo
Authors: Tanay Agrawal, Margaret E. Verrico, K. Decker French
Figure caption: (Left) GalaxyZoo classifications along with the unmatched galaxy count. (Right) Visual classifications from SDSS images, excluding the unmatched galaxies.
Paper: An Inventory of Resolved Stellar Companions in the Ariel Target List
Authors: Alex S. Polanski, Catherine A. Clark
Figure caption: Top: R.A. (azimuthal axis) versus distance in parsecs (radial axis) for stars on the Ariel target list. Black points indicate stars with no Gaia-resolved stellar companions. Blue and teal points indicate binary TOIs and known planet hosts, respectively. Diamonds represent the three systems with new candidate companions. Bottom: histograms of companion projected and angular separation with colors representing the same sub-samples as above.
Paper: Modeling Globular Cluster Counts with Bayesian Latent Models
Authors: Rafael S. de Souza, Ana L. Chies-Santos
Figure caption: Negative-binomial regression with a latent errors-in-variables treatment for the relation between NGC and ﹩{\mathrm{log}}_{10}\,({M}_{\star }/{M}_{\odot })﹩. Data points are elliptical galaxies from W. E. Harris et al. (2013). The solid blue curve shows the posterior median, and the orange band the 95% credible interval. Points include 1σ uncertainties.
Paper: The Calm before the Storm: High Spatial Resolution Mosaic of Active Region NOAA 14274 at the Onset of an X1.2 Flare
Authors: Carsten Denker, Robert Kamlah, Meetu Verma, Alexander G. M. Pietrow
Figure caption: The mosaics of speckle-restored images have a combined FOV of 240″ × 150″ and shows active region NOAA 14274 at around 08:33 UT on 2025 November 10, about 30 minutes before an X1.2 flare began. The mosaics were created using four HiFI+ channels: Ca II H λ396.8 nm, TiO λ705.8 nm, and broad- and narrow-band Hαλ656.3 nm (clockwise from the top-left panel). The FOV of the Ca II H channel (﹩48\mathop{.}\limits^{^{\prime\prime} }2\times 30\mathop{.}\limits^{^{\prime\prime} }8﹩) is too small to overlap vertically (as shown by the horizontal blue lines in the Ca II H panel), while the FOV of the other channels (﹩76\mathop{.}\limits^{^{\prime\prime} }5\times 60\mathop{.}\limits^{^{\prime\prime} }5﹩) is much larger.
Paper: A Pipeline for Generating Realistic Artificial Ultra-faint Dwarf Galaxies
Authors: Alexis H. Brown, Yao-Yuan Mao
Figure caption: Comparison between the real image of Leo K (right-hand side) and an injected replica (left-hand side). The replica was generated using parameters inferred from HST observations (K. B. W. McQuinn et al. 2024). Within each side, the top-left panel shows a zoomed-in cutout of Leo K, and the bottom-left panel displays the spatial distribution of detected sources (green points), with the black box marking the cutout region. In the right panel, orange points in the CMD represent sources that pass both the detection mask and color–magnitude selection. These points correspond to stars within the white circle of the cutout and are likely associated with Leo K. Lighter orange points are detected stars that fall outside the color cut, consistent with background sources.
Paper: Non-detection of Nightside Emission from HAT-P-26b due to Stellar Contamination
Authors: Kristin S. Sotzen, Jacob Lustig-Yaeger, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: Left: planetary infrared excess spectra from the daysides (orange and red points) and nightsides (blue and cyan points) of HAT-P-26 b. Dayside (nightside) 1 and 2 represent the pre-ingress and post-egress baseline spectra, respectively. The secondary eclipse dayside spectrum extracted using traditional methods is shown in black. The pink line and shaded regions indicate the median retrieved stellar model flux ratio with 1σ and 3σ credible intervals. Right: constraints on the change in temperature (ΔThet) and area covering fraction (Δfhet) of a heterogeneous stellar component. For HAT-P-26 b, a small change between transit and eclipse in spot properties on the stellar disk is consistent with the measured negative slope that contaminates the iESR PIE nightside spectrum, preventing assessment of any planetary emission.
Paper: Aperture-averaged Polarimetry of the Second Interstellar Comet 3I/ATLAS within the Snow Line
Authors: Maxim Zheltobryukhov, Evgenij Zubko, Mariia Tsuranova, Anton Kochergin, Ekaterina Chornaya, Gorden Videen
Figure caption: Degree of linear polarization P as a function phase angle α of the second interstellar Comet 3I/ATLAS beyond the snow line (blue points; Z. Gray et al. 2025) and within the snow line (dark red points; our observations). The four panels show different scenarios of refractory species in the 3I/ATLAS coma.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Need for Multiangle BRDF Laboratory Measurements to Model Rocky Exoplanet Surface Reflectance and Emission
Authors: Leonardos Gkouvelis
Figure caption: Schematic illustration of the secondary eclipse ingress angle for representative exoplanet configurations, including the Earth viewed as a transiting exoplanet. Small ingress angles highlight the relevance of the opposition surge.
Paper: The Lines of the Noble Gases Kr II and Xe II Formed in the Atmosphere of HR 6000 (HD 144667)
Authors: Richard Monier
Figure caption: Left: Line synthesis of the Kr II line at 4355.48 Å (observed spectrum in black, synthetic spectrum in red), Right: Line synthesis of the Xe II line at 5419.15 Å
Paper: “Dark Comet” 2005 VL1 is Unlikely to be the Lost Soviet-era Probe Venera 2
Authors: Federico Spada
Figure caption: Comparison between the orbit of 2005 VL1 (solid lines) and the trajectory of Venera 2 at launch and Venus flyby (filled squares), in terms of the distance from the Earth and from Venus (top and bottom panel, respectively). For 2005 VL1, 180 orbits are plotted, sampled from the normal distribution defined by the nominal orbital parameters and their covariance matrix obtained with orbit_finder (since the lines overlap at the scale of the main panels, zoomed-in views around the closest approach to the Earth and to Venus are provided in the insets, to give a sense of the uncertainty). Reasonable values of the uncertainty in time and distance for the Venera 2 constraints are within the size of the square symbols.
Paper: The Early Post-outburst Infrared Spectrum of the Stellar Merger V1309 Scorpii (Nova Scorpii 2008)
Authors: Richard J. Rudy, Ray W. Russell, David K. Lynch, Michael L. Sitko
Figure caption: 0.8–2.42 μm spectrum of V1309 Scorpii. The top panel shows the complete wavelength coverage to emphasize the overall spectral shape; the center and bottom panels cover the blue and red portions of the spectrum and highlight the absorption and emission features. For comparison, the top panel includes a spectrum of the F-star supergiant BD+38 2803 from the IRTF Spectral Database (Cushing et al. 2005; J. T. Rayner et al. 2009). That spectrum is adjusted to match the reddening of V1309 Sco, which is E(B − V) = 0.55 according to the study of E. Mason et al. (2010). The middle panel includes most of the emission lines present in V1309 Sco. Other than the H I lines (shown in black), the remainder (displayed in blue) are mostly from [Fe II]. Absorption lines are coded in red with the most prominent being due to [Ca II]. The bottom panel employs the same color coding and the principal spectral features are again due to H I. Possibly present are very weak absorption features from the bandheads of the first overtone of carbon monoxide (12C16O).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Sub-parsec Detectability Lifetimes for a Sample of Dual AGN with Known Mass Ratios
Authors: Colton M. Burross, Krista Lynne Smith
Figure caption: Distribution of sub-pc observability lifetime tlife for each respective Eddington ratio λ, with the mass ratio distribution of 84 double quasar pairs in displayed toward the right side within the graph.
Paper: Exploring Black Hole Accretion Through Multidimensional Simulations
Authors: David D. Vaida, Georgia Amy Richardson, Ryan Jeffrey Farber
Figure caption: The left two panels showcase the accretion rate while the right panels show the relative error between the accretion rates. The upper row of panels shows our non-viscous cases while the bottom row includes our viscous simulations. The line colors represent the linear resolution of each simulation, ranging from 64 to 2048. For the left two panels, the line styles differentiate between FLASH, Athena, and Athena++. For the right two panels, the line styles signify which two simulations we’re using to compute the relative error.
Paper: Determination of the Abundance of Mercury from the Hg II line at 5677.10 Å. XIX. HD 190229 (14 Sge)
Authors: Richard Monier
Figure caption: Left: Synthesis of the 4500–4540 Å spectral interval (observed spectrum in black, synthetic spectrum in red), Right: Synthesis of Hg II line at 5677.10 Å in one I profile of 14 Sge.
Paper: Multiwavelength SITELLE Observations of the High-velocity System in NGC 1275
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Maya Cadieux, Zachary Jean, Hyunseop Choi, Benjamin Vigneron
Figure caption: Flux maps for Hα, [N II]λ6483, Hβ and [O III]λ5007 (left to right and top to bottom). Pixels values were masked out that fell below 5×10−17 erg s−1 cm−2 Å−1 in Hα, which approximately corresponds to the 3σ noise level of the SN 3 filter observation. These figures demonstrate strong emission coming from the HVS located at approximately 8200 km s−1.
Paper: Numerical Treatment of Shock-induced Nuclear Burning in Double Detonation Type Ia Supernovae
Authors: Ryan Brady, Michael Zingale
Figure caption: (Left) Initial hydrostatic profile without the temperature perturbation Tpert = 1.14 × 109 K. (Right) Snapshot of our shock probe at t = 0.08 s across spatial resolutions of 5.0 km (top), 2.5 km (middle), and 0.3125 km (bottom). Since the burning-enabled profile overlaps the fshock = 1 profile at the finest resolution, we highlight it with data markers.
Paper: Enhanced Merger Fractions in a Reionization-era Protocluster
Authors: Lorraine C. Marcelin, Jaclyn B. Champagne, Feige Wang, Xiaohui Fan, Maria Pudoka, Wei Leong Tee, Yongda Zhu
Figure caption: (a) Gini vs. M20 in each subsample, color coded by concentration. Above the dotted line, galaxies are consistent with a merger scenario. (b) Stellar mass ratio of each merger pair (left axis) vs. median redshift. The redshift histogram of the full sample is overlaid (right axis), with shaded regions indicating overdensities. Dotted line shows the 1:3 mass ratio between major and minor mergers. (c) Half-light radius of the galaxies vs. angular distance to its nearest neighbor. Yellow stars signify close-pair mergers. Dashed line is the minimum distance criterion ﹩{r}_{p}^{{\rm{\max }}}\geqslant 100﹩ kpc. (d) 2″ × 2″  F356W cutout showing a galaxy and its merging pair (star and triangle). The [O III] emitter pair satisfies both dynamical and morphological criteria.
Paper: Variability Census of Legacy Catalogs. V. 11,820+ New δ Scuti and γ Doradus Stars
Authors: Ai-Ying Zhou
Figure caption: Example TESS light curves and periodograms of newly identified: multiperiodic γ Dor stars (top three rows: BD+47 1790, HD 117444, TYC 6553-156-1), δ Sct-γ Dor hybrid (rows 4–5: TYC 2962-1863-1, TYC 3296-2104-1). Rows 6–7: γ Dor and δ Sct pulsators blended by adjacent known eclipsing binaries.
Paper: Recent Atomic Data for Cr II Improves Non-LTE Model for Sirius A Spectrum
Authors: Katelyn R. Sonnen, Jason P. Aufdenberg
Figure caption: Synthetic lines profiles for Cr II lines (abundance ﹩{\mathrm{log}}_{10}\varepsilon ﹩ = 6.20) are displayed in comparison to the normalized VLT/UVES spectrum of Sirius A (S. Bagnulo et al. 2003). Non-LTE models with rotation (﹩v\sin i=16.7\,{\rm{km}}\,{{\rm{s}}}^{-1}﹩ C. G. Díaz et al. 2011) for lines 3084.46 Å and 3173.56 Å (top) with ﹩\mathrm{log}(gf)﹩ values from (a) R. L. Kurucz (2017) are improved (b) with values from J. W. Ward et al. (2023), ﹩\mathrm{log}(gf)=-1.006﹩ and ﹩\mathrm{log}(gf)=-1.017﹩, respectively. Non-LTE models with rotation for lines 4539.49 Å and 4565.74 Å (bottom) with ﹩\mathrm{log}(gf)﹩ values from (a) T. Wujec & S. Weniger (1981) are improved (b) with values from J. E. Lawler et al. (2017), ﹩\mathrm{log}(gf)=-2.21﹩ and ﹩\mathrm{log}(gf)=-1.84﹩, respectively. In addition, LTE models with rotation and non-LTE and LTE models without rotation are shown for comparison.
Paper: Investigating Spectral Stability in the Vicinity of the Metastable Helium Triplet of WASP-107
Authors: Chase M. Urasaki
Figure caption: Recovered EW ratios and 1σ bounds over 1000 simulations. The EW recovery improves with increasing input EW. The inset shows the MAD profile based on spectral residuals, with the He I*, Mg I, and Si I lines marked. A Savitzky–Golay filter has been applied to aid interpretation.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXII. HD 144206 (υ Her)
Authors: Richard Monier
Figure caption: Left: Synthesis of the 4460–4500 Å spectral interval (observed spectrum in black, synthetic spectrum in red), Right: Detection of the Hg II line at 5677.10 Å in the mean ELODIE spectrum of HD 144206.