adsabs/AstroCLIMB huggingface dataset:
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: CH3CN J = 173−163 moment 0 image with contours presenting the continuum emission as in Figure 2. The synthesized beam appears in the bottom right corner. The K = 3 is the strongest of the K-ladder transitions observed.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Spectra of different molecular transitions integrated over the central absorption region. The dotted black line in all the panels marks the 12.1 km s−1 systemic velocity. Top: H2S, H2CO, CH3OH, and HC3N lines. Middle: SO2 lines with E up ranging between 51 and 761 K. Bottom: several lines of the CH3CN J = 17–16 ladder. To help the readability some spectra are shifted in the y-axis, and some are also multiplied by an integer factor indicated in the legend. The two gray dotted lines mark the velocity of the two main absorption peaks at 13.5 and 16.5 km s−1, see the main text.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: CH3OH moment 0 image with contours representing the strongest continuum emission. In both panels, the solid lines represent Ulrich’s model while the dashed lines show Mendoza’s models (see the text in Section 4.3). Left panel: models using the inner equatorial radius, r in, as the molecular disk radius (357 au). Right panel: same but using r in as the envelope radius (790 au). The angles ϕ 0 and θ 0 and the parameters μ and ν of the fits are shown in Table 5. The triangles, circles, and squares mark the position of the condensations identified in the CH3OH velocity cube.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: The CH3OH position–velocity diagrams along the streamers S1, S2, and S3 (i.e., observed line-of-sight velocity vs. projected distance to the protostar location) for our best fits to the data using Ulrich’s model (solid lines) and Mendoza’s model (dashed lines). Note that the system velocity is 12.1 km s−1. Top panels: using r in as the molecular disk radius. Bottom panels: using r in as the envelope radius. The triangles, circles, and squares correspond to the S1, S2, and S3 streamers, respectively.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Sketch showing the disk, envelope, and the location of three possible accretion streamers: S1, S2, and S3. The figure indicates the approximate orientation of the thermal radio jet HH 80-81, of the disk and the system rotation. The rough representation is not to scale.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Trajectories of the S1, S2, and S3 streamers on top of the contours marking the strongest continuum emission. The line-of-sight velocity of the streamers for our best fit to the CH3OH data using Mendoza’s model is also depicted (color scale). Left panel: using r in as the molecular disk radius. Right panel: using r in as the envelope radius. The triangles, circles, and squares correspond to condensations of the S1, S2, and S3 streamers and the colors follow the same velocity color scale as the model trajectories.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Flared disk model for the H2S emission comprising three components: a compact dust disk (indicated but not shown in the sketch), a conical truncated flared molecular disk, whose lids are seen in emission, and an optically thick cold gas filling the volume between the conical lids.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Flared disk model for the H2S emission. From left to right, the images show the observed moment 0 integrated intensity image, the model obtained (see Appendix E), and the residual image after the fit. The three images have the same color scale and contours, at multiples of 10 K  km s−1. Their rms noise value is 5 K  km s−1. The beam is shown at the bottom right corner of each image.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: H2S integrated intensity image (moment 0) of the inner region of the GGD 27-MM1 disk. The color scale shows the negative absorption toward the center position. The figure shows H2S 33,0–32,1 spectra extracted and overlaid every quarter of a beam, approximately. The star marks the position of the peak of the millimeter continuum emission.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Continuum model for the continuum emission. From left to right, the images show the observed image, the model obtained, and the residual image after the fit. The three images have the same color scale and contours, at levels −25, −10, −5, 5, 10, 15, 25, 75, and 375 times the rms noise level of the image, ∼0.14 mJy beam−1.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Example of spectra fitted manually using CASSIS (pixels 3–9, 4–9, 6–7, and that of the central pixel). The observed spectra are shown by the black histograms, while the CASSIS fitting is displayed by the red curves. The top and bottom left spectra are examples of fits obtained using a single kinematical component; the top right is a fit obtained using two spectral components; the bottom right spectrum corresponds to the central pixel spectrum, which was fit using a constant background of ∼300 K, a blueshifted emitting layer and a foreground absorbing layer slightly redshifted. Note that CH3CN K = 5 is contaminated by the SO2 224,18−223,19 line (ν rest = 312.543 GHz). There are other strong lines (e.g., a CH3OH line and a SO2 line at about 312.24 GHz) in the spectra, which will be reported in another work.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in example of up to the K = 4 transition of the CH3CN spectrum fitted manually using CASSIS at the central pixel. This demonstrates the relative quality of the fit fixing the background temperature at 300 K and using two interactive emitting/absorbing layers. The observed spectrum is shown by the black histogram and the red line represents the model.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the CH3OH (31,2–20,2) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the H2S(33,0–32,1) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the CH3CN (173-163) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the HC3N(33-32) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in example of the up to K = 4 transition of the CH3CN spectrum fitted manually using CASSIS (pixel 3–7). This demonstrates the need for two kinematical components and the relative goodness of the fit. The observed spectrum is shown by the black histogram, each of the two components has its spectrum plot in gray and blue dotted lines, and the red solid line represents the total fit after adding the two components’ contributions.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the H2CO (41,3–31,2) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Zoom-in of the velocity cube image of the SO2(92,8–81,7) emission toward GGD 27-MM1. Velocity is labeled in the top left corner and the synthesized beam appears in the bottom right corner of each channel. Band 6 continuum emission contours are overlapped at levels 5, 15, and 100 times the rms.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Comparison between the orbits projected onto the plane of the sky for an inclination angle i = 0°, the inner equatorial radius r in as the envelope radius (790 au), the initial polar angle θ 0 = 30°, and different initial azimuthal angles. Left panel: Ulrich’s model. Right panel: Mendoza’s model. For Mendoza’s model, we use the parameters μ = 0.45 and ν = 0.15. The solid lines represent the infalling material, while the dashed lines denote material coming out
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Ulrich (solid lines) and Mendoza (dashed lines) orbits overlapped with moment 0 of the CH3OH 3(1,2)−2(0,2) emission. The parameters μ and ν and the angles ϕ 0 and θ 0 for the streamers S1, S2, and S3 (see Figure 9) are shown in Table 5. The models use the inner equatorial radius r in, as the molecular disk radius (357 au).
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Comparison between the orbits projected onto the plane of the sky for an initial polar angle θ = 30° and the envelope radius (r in = 790 au). Parabolic orbits, following Ulrich’s model are shown in solid lines. Conic orbits, following Mendoza’s model are shown in dashed lines. Left panel: orbits for an inclination angle with respect to the plane of the sky i = 0°. Right panel: orbits for an inclination angle with respect to the plane of the sky i = 30°. For Mendoza’s model, we consider the parameters μ = 0.45 and ν = 0.15.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Synthetic spectra (“mock data”) produced using the vis-sample routine on the time-integrated HCO+ 1–0 cubes. These models reveal any spectral or flux fluctuations that would have been introduced by varying baseline coverage for each source’s unique spatial emission structure. The subfigures show the respective analyses for (a) AS 209, (b) GM Aur, (c) HD 163296, (d) IM Lup, and (e) MWC 480. For each panel, the mock HCO+ 1–0 spectrum is shown on the left, and the mock disk-integrated continuum, line, and continuum normalized line emission are shown on the right. It should be noted that the spectra overlap.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: HCO+ J = 1–0 spectra for each of the MAPS disks with error bars for each channel. The gray error bars represent the max and mean error bars (standard deviation) for all channels. (a) AS 209. (b) GM Aur. (c) HD 163296. (d) IM Lup. (e) MWC 480.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Same figure description as Figure 3, but for MWC 480.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Same figure description as Figure 3, but for IM Lup.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by MMS. Panel (a) shows the magnetic field magnitude, (b) field components in the local LMN coordinates, (c) the total current density, (d) 2 s moving averages of J LMN components, and (e) the magnetic field divergence-curl ratio, with the dashed orange line indicating unity. In panel (c) the magenta gives the 2 s moving average of ∣J∣. The gray (teal) bars at the bottom of panels (c) and (d) indicate the times when the divergence-curl ratio was below 0.5 (1), panel (d) shows the times for the average curve.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by the Cluster 1–4 spacecraft. Panel (a) shows the magnetic field magnitude, and (b)–(f) the field components in local LMN coordinates. The blue shading in panels (a) and (b) and (e) and (f) displays the intervals that determine the normal directions. The red horizontal bar in panel (a) marks the intervals shown in panels (c) and (d). In panel (c), the pale blue curves show the B  L  rotations aligned with field increases. The pale magenta curve marks the opposite rotation discussed in the text.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME mixing layer observed on 2020 April 20. Panel (a) shows the magnetic field magnitude, (b) ϕ  B  and (c) B  Z  components from the spacecraft at the Earth’s orbit, and (d) the field magnitude at ACE, Wind, and Solar Orbiter at 1 minute time resolutions. The blue shading indicates the mixing layer characterized by large rotations of ϕ  B  and decreases in ∣B∣. In panel (d), vertical magenta lines show the ICME sheath–ejecta boundary. The spacecraft data are time shifted arbitrarily and the distance between the ticks on the horizontal axis corresponds to 1 hr.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: RGB Chandra and NuSTAR image of Cas A with a square root scale. In red, Chandra/ACIS-S count-rate image in the 4–6 keV band with a pixel size of 1″, in green the 4–6 keV NuSTAR deconvolved count-rate image, and in blue the 10–20 keV NuSTAR deconvolved image. The region used for the analysis of the whole remnant is shown in white, and the regions selected for the spatially resolved spectral analysis are shown in yellow.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Chandra and NuSTAR exposure/vignetting-corrected images of Cas A. Leftmost panel: Chandra/ACIS-S count-rate image in the 0.5–8 keV band with a pixel size of 1″ and a square root scale. Other panels: exposure/vignetting-corrected and mosaicked NuSTAR images of Cas A in various energy bands, reported on the images in units of keV, with a square root scale.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Radiation spectrum P(ω) produced by an ensemble of electron in a turbulent magnetic field (adapted from TF87). See also Reville & Kirk (2010; their Figures 5 and 6) for numerical results on the single particle emissivity. See the text for details.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by Cluster 4. Panel (a) shows the magnetic field magnitude, (b) B  L , (c) proton density, (d) velocity and the Walén prediction of V  L  from the sheath (ejecta) side on black (gray), and (e) proton temperatures.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: MMS and Cluster constellations during ICME front boundary passing on 2020 April 20. Constellation Q factors quantifying the proximity to the perfect tetrahedron (Q = 1) are shown.
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: The proof-of-concept system’s inner planet. Results of 1000 systems, represented by blue dots, integrated up to 2 Gyr of our proof-of-concept system with an Earth-mass planet introduced inward of the two observed warm Neptunes, and 220 N-body simulations, represented by green stars. The left column represents initial J 2 = 2 × 10−5, while the right column represents J 2 = 6 × 10−4; these two values represent the bottom and top curves, respectively, in Figure 1. The top row indicates for each run the minimum value of δ (see Equation (17)) achieved over the entire run. The shaded regions represent regions of instability, either from Roche limit crossing (left) or orbit crossing indicated by δ = 0 (right). The middle row indicates the maximum eccentricity achieved by the inner planet over each run. The bottom row indicates the maximum mutual inclination between the inner planet and the two warm Neptunes over the course of the run. The red curve indicates the maximum mutual inclination that the inner planet can have with its closest neighbor and still transit.
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: Top row: eccentricity and mutual inclination with middle planet as a function of time for a run from the Monte Carlo described in Section 5.2. An inner planet was inserted into the proof-of-concept system with initial conditions a in = 0.02061, e in = 0.08247, i in = 1.°07865, and Ωin = 154.°6. Representative of the effect of sweeping resonances is the swift transition in the inclination of the inner planet as a resonance passes through it at ∼40  Myr. The rolling average of the inclination of the middle planet remains at ∼2.°5 over the entire integration, with the magnitude of its inclination oscillations changing from ±4° to ±0.°5 after the inner planet transitions to its higher mutual inclination state. The slower climb of the eccentricity evolution is caused by the fact that the inner planet’s semimajor axis corresponds to a resonance when J 2 ∼ 0, meaning that as J 2 decreases over the whole integration, the predicted eccentricity slowly increases, rather than suddenly transitioning. Bottom row: difference of Ω and ϖ angles between the inner and middle planets as a function of time. The alignment of angles during the resonances is shown by the large gaps occurring at the same time as the transitions to higher eccentricity and inclination.