adsabs/AstroCLIMB huggingface dataset:
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: A comparison between the best-fit central wavelengths calculated for each experiment. Both use a single-Gaussian model and are fit with their wavelengths as measured in air. The middle panel converts the visual spectroscopic redshift, VI_Z, to an Lyα or [O II] wavelength value redshifted to the observed frame and compares to the best-fit wavelength in the DESI data. The bottom panel presents a comparison between HETDEX spectroscopic redshifts and DESI VI spectroscopic redshifts.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Line flux comparison for the 982 LAEs detected by HETDEX that are confirmed by DESI (VI_QUALITY ≥ 3) is shown in the top panel, and the error-weighted difference is shown in the bottom panel. Data points are separated based on HETDEX line width values, SIGMA_HETDEX. As demonstrated in the bottom panel of Figure 7, asymmetric and double-peaked line profiles are fit with higher line widths in the HETDEX spectra, resulting in higher Lyα flux values.
Paper: DESI Spectroscopy of HETDEX Emission-line Candidates. I. Line Discrimination Validation
Authors: Martin Landriau, Erin Mentuch Cooper, Dustin Davis, Karl Gebhardt, Robin Ciardullo, Éric Armengaud, Arjun Dey, Anand Raichoor, David J. Schlegel, Michael Wilson, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, L. Le Guillou, Michael E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, I. Pérez-Ràfols, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou, Daniel J. Farrow, Gary J. Hill, Donghui Jeong, Chenxu Liu, Shun Saito, Donald P. Schneider
Figure caption: Comparison of Gaussian line width (σ) values between DESI (y-axis) and HETDEX (x-axis). Both line profiles are modeled using a single-Gaussian model. HETDEX values are corrected for the lower instrumental resolution of the VIRUS spectrograph compared to the DESI spectrograph. The values show large scatter at higher line width, where the difference in spectral resolution can lead to fitting of only one peak in the double-peaked and asymmetric lines found in the LAE sample.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Electron energy spectra for Runs III and IV for the entire domain. The particle energy is scaled by the magnetization, and ﹩f(\gamma )﹩ is defined such that ﹩\int f(\gamma )d\gamma =1﹩ (since we plot the probability density per γ and not γ/σ, the integrals of the plotted curves differ by a factor of σ). The dashed blue line indicates the expected pickup energy, ﹩m{v}_{{\rm{A}}}^{2}﹩. The transition between the exhaust component and the plasmoid component is indicated by the yellow line. Note that the first structures on the far left for each case represent the inflow, which has acquired a small thermal temperature due to wave heating. As the domain size (Ly) grows for σ = 0.3, the shape of the plot looks the same, however the magnitude of the plasmoid component in the spectrum decreases relative to that of the exhaust due to the decreasing fraction of the domain occupied by plasmoids.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Spacetime plots of the midline (x = Lx/2 = 60 c/ωp) for Runs I and II, respectively, after they have reached equilibrium. The areas with the lowest density (the darkest blue) are the diffusion regions, and the high-density streaks of yellow are the plasmoids—thus these plots show the life journey of plasmoids as they are born and leave the domain. As one can see in the σ = 0.3 case, plasmoid production, while regular, is sufficiently infrequent to allow most plasmoids to escape the X-point at the center without ever merging with another plasmoid (though one prominent collision can be seen near (190, 180)). The case in Run I is quite different; here we see rapid plasmoid production and, crucially, many mergers. This results in large, slow plasmoids which themselves are more susceptible to further mergers. This feedback mechanism fills the domain with large, massive plasmoids.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Plots (a)–(h) show selected quantities for a cut along y = 1600 c/ωp in Run V. Plots (a) and (b) show the normalized density and normal bulk velocity, respectively. Plots (c)–(h) show the Rankine–Hugoniot jump quantities, normalized to their upstream values. Plot (i) shows general quantities plotted along that same y-value; the transition region depicted in plots (a)–(h) is shaded in gray. The upstream magnetic pressure ﹩{P}_{B0}\equiv {B}_{0}^{2}/8\pi ﹩.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Density profiles for Runs III and IV, respectively, once steady state is achieved. The density scale is cut off at 5 times the inflow density.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: X-points from Runs I and II. The nonideal electric field Eni ≡ E + v × B/c in the out-of-plane direction is plotted. The E = (vA/c)B contours, giving the boundaries of the diffusion region for the purposes of computing the exit spectra, are shown in yellow.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Normalized kinetic energy values for tracked simulation electrons upon their departure from the primary diffusion region, summed over time. The dotted line shows the analytical expression for the nonrelativistic exit spectrum (Equation (15)). The humps seen in the curve for σ = 0.3 are caused by a Hall-like Ex component noted by M. Swisdak et al. (2008) which results in step-wise acceleration and bunches up the electron distribution; see Appendix C for details. From left to right, the peaks correspond to particles which complete one, two, and three Speiser oscillations before leaving the diffusion region.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Trajectory of an electron over the density profile for the last time step plotted for Run II (σ = 0.3). Ω is the upstream electron gyrofrequency. The particle first interacts with the current sheet at the X-point (105 ≲ Ωt ≲ 120) and is thereafter confined within a plasmoid (Ωt ≳ 120). As the plasmoid and trapped electron move together into the outflow, the electron energy initially imparted by direct E-field energization is magnified several times by Fermi/betatron heating. The oscillation in energy reflects the gyration up and down the Ez potential.
Paper: Transition to Petschek Reconnection in Subrelativistic Pair Plasmas: Implications for Particle Acceleration
Authors: Adam Robbins, Anatoly Spitkovsky
Figure caption: Hall-like electric fields near the diffusion region, with magnetic field lines overlaid in black.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Mean differential source counts derived from 200 simulated realizations, estimated using three methods: the traditional binned approach (orange), standard KDE (blue), and adaptive KDE (red). In each panel, the green dashed line shows the true source counts computed from Equation (14), and the shaded regions indicate the 1σ dispersion across the 200 samples. The flux limit adopted in each case is marked by a vertical dotted line. In the binned method, we divide the logarithmic flux density space into equal-width bins according to Scott’s rule, with the number of bins indicated in each panel.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Differential source counts for the three LoTSS Deep Fields (Lockman Hole, Boötes, and ELAIS-N1) obtained with the traditional binned estimator. Black filled squares show the results of S. Mandal et al. (2021), and red filled circles show our own estimates. The binning scheme follows S. Mandal et al. (2021) with slight shifts in several bin edges, illustrating the sensitivity of histogram-based estimators to bin placement.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Differential source counts for the three LoTSS Deep Fields, estimated using the adaptive KDE method (solid red lines). The pale-red shaded region indicates the 3σ uncertainty band for the KDE estimate. For comparison, the binned results from S. Mandal et al. (2021) are shown as black squares.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Similar to Figure 4, black squares denote the results of S. Mandal et al. (2021), and dark-green circles show our estimates using the Bayesian Blocks adaptive binning algorithm.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Similar to Figure 1, except that here the differential source counts are estimated using the adaptive binning method based on the Bayesian Blocks algorithm (J. D. Scargle et al. 2013). In this approach, the bin widths vary with the local data density.
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Distributions of the discrepancy metric dn for different source count estimators, based on 200 simulated samples at each flux limit. Each panel corresponds to a different flux threshold.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Intensity-weighted mean velocity (moment 1) map of (a) HCN J = 4–3, (b) HCO+ J = 4–3, (c) HCN J = 3–2, and (d) HCO+ J = 3--2, created with 1.5 mas pixel−1. The displayed velocity range is 1130﹩{}_{-170}^{+320}﹩ km s−1 (960–1450 km s−1) for (a)–(d), to clearly display the innermost (≲1 pc) high-velocity redshifted HCN emission in the western torus (e.g., C. M. V. Impellizzeri et al. 2019; M. Imanishi et al. 2020) (see text in Section 3). Moment 1 maps of (e) HCN J = 4–3 and (f) HCN J = 3–2 are shown with the velocity ranges of 1130±110 km s−1 (= 1020–1240 km s−1) and 1130 ± 60 km s−1 (= 1070–1190 km s−1), respectively, to display overall redshifted and blueshifted motion of the torus dense molecular gas emission with respect to the systemic velocity (Vsys = 1130 km s−1). The plus mark is the ∼350 GHz continuum emission peak position (02h 42m 40﹩\mathop{.}\limits^{{\rm{s}}}﹩709, −00°00﹩{}^{{\prime} }﹩ 47﹩\mathop{.}\limits{^{\prime\prime} }﹩946)ICRS defined as C-peak. The open diamond mark is the emission peak in the western torus in the HCN J = 4–3 moment 0 map (02h 42m 40﹩\mathop{.}\limits^{{\rm{s}}}﹩7084, −00°00﹩{}^{{\prime} }﹩ 47﹩\mathop{.}\limits{^{\prime\prime} }﹩940) ICRS defined as W-peak. The horizontal thick black bar at the bottom center of each panel corresponds to 1 pc at the distance of NGC 1068. The open circle at the lower-left part of each panel indicates the synthesized beam size, which is 0﹩\mathop{.}\limits{^{\prime\prime} }﹩014 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩013 (≲1 pc) for the J = 4–3 lines of HCN and HCO+, and 0﹩\mathop{.}\limits{^{\prime\prime} }﹩020 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩018 for the J = 3–2 lines. An appropriate cutoff (∼4.5σ) is applied to all the moment 1 maps to prevent them from being dominated by noise.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Velocity profile of (a) HCN J = 4–3, (b) HCO+ J = 4–3, and (c) HCN-VIB J = 4–3 line in the beam-sized spectrum toward the ∼350 GHz continuum emission peak ("C-peak"). The abscissa is the optical LSR velocity (in km s−1) and the ordinate is the flux density (in mJy beam−1). A downward arrow is added at the systemic velocity of NGC 1068 (Vsys = 1130 km s−1), labeled as “Vsys.” The horizontal thin dotted straight line indicates the zero-flux level. In (b), an upward arrow is added at the velocity of V = 1530 km s−1 (Vsys + 400 km s−1) to indicate an absorption feature that is 400 km s−1 redshifted relative to the systemic velocity. In (c), a red upward arrow is added at the velocity of V = 1470 km s−1 (Vsys + 340 km s−1) to indicate redshifted emission at the innermost (≲1 pc) western torus (see Section 3).
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Intensity-weighted velocity of the HCN J = 4–3 (open circles) and 22 GHz (1.4 cm) H2O maser emission (red filled triangles) (ordinate) as a function of distance from the SMBH position (continuum emission peak) along the NW direction (PA = 135°) (abscissa). We shift our ALMA HCN J = 4–3 data by ∼9 mas (∼0.65 pc) toward the NW direction (see also V. Gamez Rosas et al. 2025), assuming that the most highly redshifted (V ∼ 1470 km s−1 or ΔVred ∼ +340 km s−1) HCN J = 4–3 emission component is at ∼0.5 pc from the VLBI 22 GHz continuum emission peak, where the 22 GHz H2O maser emission also displays the most redshifted components with V ∼ 1470 km s−1 (ΔVred∼ +340 km s−1) (J. F. Gallimore & C. M. V. Impellizzeri 2023). This is because the continuum emission peak positions often do not perfectly agree between ALMA at ∼260–350 GHz and VLBI at ∼22 GHz, possibly due to nonperfect astrometric accuracy. Red filled triangles: 22 GHz H2O maser emission. Data in the R1, R2, and R3 regions, and those with >1450 km s−1 in the R4 region (J. F. Gallimore & C. M. V. Impellizzeri 2023) are plotted. Distance in the abscissa is calculated from the offset values from the S1 in Table 1 of J. F. Gallimore & C. M. V. Impellizzeri (2023). Open circles: HCN J = 4–3 emission with 2 pixel width. The horizontal dotted straight line indicates the systemic velocity of Vsys = 1130 km s−1. The counterrotation signature, with a velocity change from redshifted at ≲2 pc to blueshifted at ≳2 pc, is seen along the NW direction.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Observed beam-sized spectra at (a) ∼350 GHz continuum emission peak (02h42m40﹩\mathop{.}\limits^{{\rm{s}}}﹩709, −00°00﹩{}^{{\prime} }﹩ 47﹩\mathop{.}\limits^{\unicode{x02033}}﹩946) ICRS (defined as “C-peak”), (b) HCN J = 4–3 emission peak in the western torus (02h42m40﹩\mathop{.}\limits^{{\rm{s}}}﹩7084, −00°00﹩{}^{{\prime} }﹩47﹩\mathop{.}\limits^{\unicode{x02033}}﹩940) ICRS (defined as “W-peak”), and (c) HCN J = 4–3 emission peak in the eastern torus (02h42m40﹩\mathop{.}\limits^{{\rm{s}}}﹩710, −00°00﹩{}^{{\prime} }﹩47﹩\mathop{.}\limits^{\unicode{x02033}}﹩946) ICRS (defined as “E-peak”). The abscissa is the observed frequency (in GHz) and the ordinate is the flux density (in mJy beam−1). The beam size is 0﹩\mathop{.}\limits{^{\prime\prime} }﹩014 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩013 (0.98 pc × 0.91 pc). Downward arrows indicate the expected frequency of HCN J = 4–3 (νrest = 354.505 GHz), HCO+ J = 4–3 (νrest = 356.734 GHz), and HCN-VIB J = 4–3 (νrest = 356.256 GHz) lines for the systemic optical LSR velocity of NGC 1068, Vsys = 1130 km s−1 (e.g., M. Imanishi et al. 2016a, 2018b; C. M. V. Impellizzeri et al. 2019; M. Imanishi et al. 2020; J. F. Gallimore et al. 2024). The horizontal dotted straight line indicates the zero-flux level.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Integrated-intensity (moment 0) map of (a) HCN J = 4–3, (b) HCO+ J = 4–3, (c) HCN J = 3–2, and (d) HCO+ J = 3–2, created with a pixel scale of 1.5 mas pixel−1. The gray contours indicate simultaneously obtained continuum emission with 50σ, 70σ, 90σ, and 110σ ((a)–(b) at ∼350 GHz) and 40σ, 60σ, and 80σ ((c)–(d) at ∼260 GHz), where the 1σ value is shown in Table 2. The horizontal thick black bar at the bottom center of each panel corresponds to 1 pc at the distance of NGC 1068. The filled white circle at the lower left of each panel indicates the synthesized beam size, which is 0﹩\mathop{.}\limits{^{\prime\prime} }﹩014 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩013 for the J = 4–3 lines of HCN and HCO+ (a–b), and 0﹩\mathop{.}\limits{^{\prime\prime} }﹩020 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩018 for the reanalyzed images of the J = 3–2 lines (c–d).
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Upper panels: Observed area-integrated spectra of HCN J = 4–3 and HCO+ J = 4–3, extracted with (a) a 1.7 pc (24 mas) diameter circular aperture centered at the W-peak, (b) a 1.7 pc diameter circular aperture centered at the E-peak, (c) a 3.4 pc (48 mas) diameter circular aperture centered at the C-peak, and (d) a 6.8 pc (96 mas) diameter circular aperture centered at the C-peak. Lower panels: Observed area-integrated spectra of HCN J = 3–2 and HCO+ J = 3–2, extracted with (e) a 1.7 pc (24 mas) diameter circular aperture centered at the W-peak, (f) a 1.7 pc diameter circular aperture centered at the E-peak, (g) a 3.4 pc (48 mas) diameter circular aperture centered at the C-peak, and (h) a 6.8 pc (96 mas) diameter circular aperture centered at the C-peak. The abscissa is the observed frequency (in GHz) and the ordinate is the flux density (in mJy). Downward arrows are added at the expected frequencies of the HCN, HCO+, and HCN-VIB lines at J = 4–3 and J = 3–2, corresponding to the systemic velocity of Vsys = 1130 km s−1. The horizontal dotted straight line indicates the zero-flux level.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Position–velocity diagram of (a) HCN J = 4–3, (b) HCO+ J = 4–3, (c) HCN J = 3–2, and (d) HCO+ J = 3–2 lines, along the position angle of PA = 114°east of north. The abscissa is the offset from the ∼260–350 GHz continuum emission peak (in pc). West is to the right and east is to the left. The ordinate is the optical LSR velocity (in km s−1).
Paper: Improving Radio Source Count Estimation Using Kernel Density Estimation
Authors: Luozhenhan Liu, Zunli Yuan, Wenjie Wang, Chuanqi Li
Figure caption: Posterior distributions of the adaptive KDE parameters h0 and β, derived with the routine AstroKDE. Panels from left to right show the three LoTSS Deep Fields: Lockman Hole, Boötes, and ELAIS-N1.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Left: 1.3 M⊙ classical (gray) and accreting evolutionary tracks (black). Only intrinsic luminosity is drawn here, meaning that Lacc (Equation (6)) is not included. Symbols highlight key windows during the pre-MS evolution; the depletion of 2H, the depletion of 12C, and the ZAMS. The latter two are made visible with an inset figure, and the accretion phase is also indicated with arrows. Right: classical and selected accreting evolutionary tracks in the HR diagram. Again, only intrinsic luminosities are drawn here, meaning that Lacc (Equation (6)) is not included. Evolutionary tracks are drawn until the central hydrogen abundance drops 0.1% from its initial value. A luminosity burst in the 1.6 M⊙ model is also indicated with an arrow.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: (a): Integrated-intensity (moment 0) map of the CS J = 7–6 line. In the same way as in Figure 1(a), (i) the gray contours indicate simultaneously obtained ∼350 GHz continuum emission with 50σ, 70σ, 90σ, and 110σ, (ii) the horizontal thick black bar corresponds to 1 pc at the distance of NGC 1068, and (iii) the filled white circle indicates the synthesized beam size with 0﹩\mathop{.}\limits{^{\prime\prime} }﹩014 × 0﹩\mathop{.}\limits{^{\prime\prime} }﹩013. Observed area-integrated spectra around the CS J = 7–6 line with (b): a 1.7 pc (24 mas) diameter circle centered at the W-peak, (c): a 1.7 pc diameter circle centered at the E-peak, and (d): a 3.4 pc (48 mas) diameter circle centered at the C-peak. The abscissa is the observed frequency (in GHz) and the ordinate is the flux density (in mJy). Downward arrows are added at the expected frequency of the CS J = 7–6 (νrest = 342.883 GHz) for the systemic velocity of Vsys = 1130 km s−1. The horizontal dotted straight line indicates the zero-flux level.