adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: An assessment of the relationship between magnetic field and intensity structure (as a proxy for column density) in the Eos cloud. Upper: Planck magnetic field vectors plotted on the Planck Stokes I map. Vectors used in the HRO analysis are shown in black and bold. Other vectors are plotted more faintly. Contours of Stokes I are plotted at intensities of 50, 80, 120, 200, and 300 μKRJ. Lower: HRO (J. D. Soler et al. 2013, 2017) of the selected vectors in the upper panel, showing a clear tendency for magnetic fields to run parallel to intensity structure.
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: Background of the left panel is the Planck Stokes I map. Selected vectors are in bold and black, with a selection criteria of I > 40 μKRJ. Nonselected vectors are fainter. The region shown in Figure 7 is shown in the black box. The SF of the selected vectors is shown on the right (R. H. Hildebrand et al. 2009).
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: Moment 0 map from the GALFA-H I data. The gray contour shows the boundary of the cloud from the UV observations. Black contours are the same as Figure 4.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Evolution of the mass ratio (panel (a)), orbital period (panel (b)), and mass-transfer rate (panel (c)) as a function of the mass-transfer timescale (t − trlof, trlof is the stellar age when the Roche-lobe overflow occurs) for MS binary systems with (M1, M2) = (3.0, 2.0) M⊙. The purple curve corresponds to the initial orbital period Pi = 0.68 days under the standard MB law (i.e., Bs = 0 G). The black, blue, and green curves correspond to Pi = 1.4 days and Bs = 2000 G, 5000 G, and 15,000 G, respectively.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Evolution of the evolved stars in four MS binary systems in the H-R diagram. The black, blue, green, and purple curves correspond to the evolutionary tracks of MS binary systems A(M1/M⊙, M2/M⊙, Pi/days, Bs/G =  2.6, 1.2, 4.2, and 8000), B(2.7, 1.4, 7.0, and 16,000), C(3.3, 1.9, 3.4, and 13,000), and D(4.0, 3.0, 6.0, and 15,000), respectively. The bold curves represent the orbital decay stages. The solid red circles with error bars denote the locations of the five Algol binaries in Table 1.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Same as in Figure 2, but only for systems characterized by evolved stars with fixed surface magnetic field Bs = 13,000 G. The black, blue, and green curves correspond to the initial orbital periods Pi = 1.4, 2.4, and 3.4 days, respectively.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Same as in Figure 3, but for the evolution of evolved stars in the H-R diagram. The bold curves represent the orbital decay stages. The red solid circles and red crosses represent the onset at which the RLOF and the reversal of mass ratio take place, respectively.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Evolution of the orbital period as a function of mass ratio for the same three systems with Ap/Bp components as in Figure 2. Here, the standard MB law (i.e., Bs = 0 G) was ignored. The red solid circles denote the first minimum orbital periods.
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: Same as Figure 6. Planck CO (1–0) contours are overlaid in white. Selected vectors are plotted (in black) within the masked area from the CO emission found in T. M. Dame & P. Thaddeus (2022). The SF of the black vectors is shown on the right (R. H. Hildebrand et al. 2009).
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Same as in Figure 4, but only for systems characterized by evolved stars with fixed surface magnetic field Bs = 13,000 G. The black, blue, and green curves correspond to initial orbital periods Pi = 1.4, 2.4, and 3.4 days, respectively.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Relation between the function f(q, β) and the mass ratio q. The dotted, solid, and dashed lines describe the cases with β = 1.0, 0.9, and 0.8, respectively. The horizontal red line denotes f(q, β) = 0, over which the mass transfer would produce an orbital expansion effect.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Same as in Figure 7, but for a comparison between our simulated results and the observed parameters in ﹩-\dot{P}﹩ vs. the mass-transfer timescale (t − trlof) diagram.
Paper: Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?
Authors: Guan-Long Wu, Zhao-Yu Zuo, Wen-Cong Chen
Figure caption: Same as in Figure 7, but for the evolution of the stellar-wind-loss rates of evolved stars as a function of the mass-transfer timescale (t − trlof).
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Color–color diagrams for NGC 2808, with stars hued by evolutionary phase: MS in orange, GB in teal, RHB in red, BS in blue, BHB in magenta, and EHB in cyan. These indicate that each evolutionary phase occupies a distinct locus in multiband color space. Bottom right: histogram showing the distribution of distances between observed and synthetic colors, normalized by the number of stars in each evolutionary phase. This quantifies the tightness of the match. The color scheme follows that of the other panels.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: SSP spectra for NGC 2808, including the base model (gray solid line) and models with additional contributions from the BS (blue dotted–dashed line) that closely match the base model, BHB (cyan dashed), and EHB (magenta dotted) stars. The final composite spectrum, including all components, is also shown as a black solid line. The bottom panel displays the residuals with respect to the base model (Fi − Fbase), highlighting the relative flux contributions of each hot stellar component.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: CMDs of NGC 2808, with stars color-coded by evolutionary subset: MS (orange right-facing triangles), GB (teal upward-facing triangles), RHB (red left-facing triangles), BS (blue squares), BHB (cyan points), and EHB (magenta stars). These show how CMDs in different bands are varied in morphology, particularly the BHB and EHB.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Integrated spectra for each evolutionary phase of NGC 2808, color-coded as follows: MS (orange), GB (teal), RHB (red), BS (blue), BHB (cyan), and EHB (magenta). Note that BHB and EHB are as important as MS and GB in the blue wavelengths (below 3000 Å).
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Integrated spectra for each evolutionary phase of M 2, color-coded as follows: MS (orange), GB (teal), RHB (red), BS (blue), BHB (cyan), and EHB (magenta). Note that this plot covers bluer wavelengths than Figure 5, and in this case, BHB and EHB dominate the UV flux (below 1500 Å).
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Color–color diagrams and histogram of the distribution of normalized distances between observed and synthetic colors for M 2, with stars hued by evolutionary phase following the same scheme as in Figure 3.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: CMDs of M 2, with stars color-coded by evolutionary subset, following the same scheme as in Figure 1.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Top Panel: SED fitting for the white dwarf SDSS J113907.57+511103.6. The best-fit DA white dwarf model (purple) is compared to optical photometry from u, g, r, i, z (black) and G, BP, RP (orange diamonds). While the model closely matches the u, g, r bands, significant deviations are present at i, z and RP (high outliers), as well as BP and G (low outliers). An IR excess is detected at J (blue) just above 3σ and W1, W2 (green) bands. Bottom Panel: Residuals expressed in units of measurement uncertainty (σ), with red dashed lines indicating the ±3σ threshold for identifying significant excess or deficit in the observed flux.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Residuals of the synthetic base SSP (in black), all SSP (in magenta), and 11.5 Gyr BC03 SSP (in green) compared to the observed integrated spectrum of M 2 from IUE (V. Caloi et al. 1983) and Blanco Telescope (R. P. Schiavon et al. 2005), represented by the gray zero line, ranging from the far-UV to the optical regions. Much like in Figure 10, our all SSP presents an overall lower residual compared to the others.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Residuals of the synthetic base SSP (in black), all SSP (in magenta), and 11.5 Gyr BC03 SSP (in green) with respect to the observed integrated spectrum of NGC 2808 from the Blanco Telescope (R. P. Schiavon et al. 2005), represented by the gray zero line, spanning the optical region. The residuals are lower for our all SSP.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: SSP spectra for M 2, including different hot stellar components and residuals (Fi − Fbase), following the same color scheme as in Figure 7. While the BS still have a small contribution around 2000 Å, the extended wavelength coverage into the far-UV allows a direct comparison of the relative flux contributions from BHB and EHB stars.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Synthetic all SSP in magenta compared to the observed integrated spectra of M 2 from IUE (V. Caloi et al. 1983) in blue, red, and yellow, covering the far-UV normalized to 2750 Å, and Blanco Telescope (R. P. Schiavon et al. 2005) in gray, covering the optical normalized to 4995 Å.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Synthetic all SSP in magenta compared to the observed integrated spectrum of NGC 2808 from the Blanco Telescope (R. P. Schiavon et al. 2005), shown in gray, covering the optical region and normalized to 1 at wavelength 4995 Å. The drops in observed flux at the extremes are due to instrumental effects.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Contour plot of the S values computed by comparing all the DA models in our grid to the observed spectrum of the star SDSS J113907.57+511103.6. The red star represents the “hot” solution, while the blue star corresponds to the “cold” solution, reflecting the degeneracy in the Balmer line fitting technique.
Paper: Hidden Figures of Globular Clusters: Integrated Stellar Populations Impacted by Hot Subdwarfs
Authors: Thayse A. Pacheco, Paula R. T. Coelho, Lucimara P. Martins, Ricardo P. Schiavon, Erik V. R. de Lima, Marcos P. Diaz, Domenico Nardiello, Ronaldo S. Levenhagen, Rogério Riffel, Charles J. Bonatto, Ana L. Chies-Santos
Figure caption: Photometric completeness after applying our selection criteria in the NGC 7089 HST data, hued by the rainbow (where red represents 100% complete) for positions on the left and UV CMD for positions on the right.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: SED of SDSS J113907.57+511103.6, showing photometric observations (black and green points with error bars) overlaid with the best-fitting composite spectral model (brown). The individual contributions from the white dwarf (TLUSTY model, green line) and the M-dwarf companion (ATLAS model, blue line) are also shown. Filter transmission curves for GALEX, SDSS, Gaia, 2MASS, and WISE bands are shaded in the background. The WISE W3 and W4 band fluxes are affected by zodiacal foreground emission. The model successfully reproduces both the ultraviolet and optical flux, as well as the infrared excess, confirming the presence of a cool main-sequence companion. The theoretical composite SED was normalized to the observed data in the SDSS u band at 3519 Å. For comparison, an 11,000 K WD model is shown (PET, brown dashed line) from the synthetic spectral library of P. E. Tremblay et al. (2013).
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Example of our DB white dwarf fitting procedure for SDSS J181204.26+650452.6, the only DB white dwarf in our data set. Top Left Panel: The observed spectrum (black) with the flux calibration function is applied to determine the continuum. The red line represents the scaled model used for this calibration step. Bottom Left Panel: The normalized spectrum after dividing by the continuum function, showing the absorption features in relative flux units. Right Panel: The best-fit models overlaid on the observed spectrum, with the “hot” solution (Teff = 40,961 K, ﹩{\mathrm{log}}\,g﹩ = 7.73, ﹩{\mathrm{log}}\,{\rm{H}}/\mathrm{He}﹩ = −2.16) shown in red and the “cold” (Teff = 16,828 K, ﹩{\mathrm{log}}\,g﹩ = 8.02, ﹩{\mathrm{log}}\,{\rm{H}}/{\rm{He}}﹩ = −6.39) in blue. The models are offset for clarity, and the inset highlights the Hβ region (4681–5100 Å) used for determining the hydrogen abundance.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Example of our DA fitting procedure for SDSS J113907.57+511103.6. Top Left Panel: Best “cold” solution for Balmer line fitting, observed Balmer line profiles (black) and best model (blue) with Teff = 11,154 K and ﹩{\mathrm{log}}\,g﹩ = 8.70. Top Right Panel: Full observed spectrum with the best cold model fitting, normalized at 4600 Å. Bottom Left Panel: Best hot solution for Balmer line fitting, observed Balmer line profiles (black), and the best model (red) with Teff = 19,332 K and ﹩{\mathrm{log}}\,g﹩ = 8.00. Bottom Right Panel: Full observed spectrum with the best hot model fitting, normalized at 4600 Å.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Mass distribution histogram for the infrared-excess DA white dwarfs in our sample. The distribution shows a mean mass of 〈M〉IR = 0.78 M⊙, indicating a tendency toward higher-mass white dwarfs compared to the local DA population within 40 pc.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Contour plot of the photometric fit using the u, g, and r bands for SDSS J113907.57+511103.6. The fit is more sensitive to Teff than ﹩{\mathrm{log}}\,g﹩, with the best-matching model at Teff = 17,193 K and ﹩{\mathrm{log}}\,g﹩ = 7.49 noted by the red star. The photometric constraints aided in selecting the preferred spectroscopic solution.
Paper: White Dwarfs with Infrared Excess in the HET Dark Energy Experiment
Authors: Rudy A. Morales, Barbara G. Castanheira, Jayden Blanchard, Detlev Koester, Péter Németh, S. O. Kepler, Erin Mentuch Cooper, Karl Gebhardt
Figure caption: Contour plot of the S values computed by comparing all the pure DB models in our grid to the observed spectrum of the star SDSS J181204.26+650452.6, showing a similar degeneracy, with the red and blue stars marking the “hot” and “cold” solutions, respectively.
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Comparison between experimental IR spectra of ﹩{{\rm{C}}}_{70}^{+}﹩ recorded by helium-tagging (this work; black) and in a neon matrix (digitized from B. Kern et al. 2016; blue). Experimental spectra are complemented with DFT calculations carried out at the B3LYP/6-311G* level of theory and convolved with Lorentzian functions with an FWHM of 10 cm−1 (purple). The geometry optimization and frequency analysis of ﹩{{\rm{C}}}_{70}^{+}﹩ were done in the Cs point group.
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Bottom: Individual spectra of ﹩{{\rm{C}}}_{60}^{+}﹩ (black), ﹩{{\rm{C}}}_{70}^{+}﹩ (red), C60 (blue; digitized from J. P. Hare et al. 1991), and C70 (purple; digitized from V. Schettino et al. 2002). Spectra have been individually normalized to the most intense absorption feature in the region presented and have been offset vertically for clarity. Top: A comparison of the continuum-subtracted Spitzer infrared spectrograph observed emission spectra from Tc 1 (blue; digitized from J. Bernard-Salas et al. 2012) and SMP LMC 56 (red; digitized from J. Bernard-Salas et al. 2012) to the summed absorption spectrum of ﹩{{\rm{C}}}_{60}^{+}﹩, ﹩{{\rm{C}}}_{70}^{+}﹩, C60, and C70 (black).
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Photofragmentation spectrum of ﹩{{\rm{C}}}_{60}^{+}-{\rm{He}}﹩ (black) and ﹩{{\rm{C}}}_{60}^{+}-{{\rm{He}}}_{2}﹩ (red). The ﹩{{\rm{C}}}_{60}^{+}-{{\rm{He}}}_{2}﹩ spectrum is offset vertically for clarity and shows a redshift of less than 1 cm−1 compared to ﹩{{\rm{C}}}_{60}^{+}-{\rm{He}}﹩.
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Comparison between experimental IR spectra of ﹩{{\rm{C}}}_{60}^{+}﹩ recorded by helium-tagging (this work, black; digitized from D. Gerlich et al. 2018, red) and in a neon matrix (digitized from B. Kern et al. 2013, blue). Experimental spectra are complemented with DFT calculations carried out at the B3LYP/6-311G* level of theory and convolved with Lorentzian functions with an FWHM of 10 cm−1 (purple).
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Calculated IR spectrum of ﹩{{\rm{C}}}_{60}^{+}﹩ in D5d symmetry using the B3LYP/6-311G* functional and basis set. The stick spectrum has been convolved with Lorentzian functions with an FWHM of 10 cm−1.