adsabs/AstroCLIMB huggingface dataset:
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Perp-Type: velocity gradient direction ⊥ outflow direction (67.°5 ≤ ∣θ Out − θ  v ∣ ≤ 90°). First column: 870 μm dust polarization intensity in color scale overlaid with the redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), polarization segments, and dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the B-field segments (i.e., polarization rotated by 90°) and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. In the second and third panels, the black segments represent the B-fields. The red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. The gray arrows in the second and third columns indicate the mean B-field directions weighted by the intensity including all the polarization segments and weighted by the uncertainty within an annular region of 400–1000 au, respectively. In all panels, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed and solid circles correspond to scales of 1000 and 400 au, respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Self-scattering-dominated protostars. First column: 870 μm dust polarization intensity in color scale overlaid with redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), the polarization segments, and the dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the polarization segments and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. The magenta arrow indicates the mean polarization direction weighted by the intensity within the inner region of 400 au. In the second and third panels, the red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. In all panels, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed circles correspond to a scales of 1000 au. The black solid circle indicates the disk size of the protostars, obtained from Tobin et al. (2020).
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Unres-Type (26 including HOPS-250): velocity gradient is unresolved. First column: 870 μm dust polarization intensity in color scale overlaid with the redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), polarization segments, and dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the B-field segments (i.e., polarization rotated by 90°) and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. In the second and third panels, the black segments represent the B-fields. The red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. The gray arrows in the second and third columns indicate the mean B-field directions weighted by the intensity including all the polarization segments and weighted by the uncertainty within an annular region of 400–1000 au, respectively. In all panels, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed and solid circles correspond to scales of 1000 and 400 au, respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: CDF of the projected angles. The red polyline is the observed angle difference between the outflow direction θ Out and uncertainty-weighted mean B-field direction 〈θ  B 〉 σ . The black solid line, dashed line, and dotted–dashed line indicate Monte Carlo simulations of the expected projected angle for two vectors that are 3D random (difference angle of two vectors is between 0°and 90°), parallel (0°–22.°5), and perpendicular (67.°5–90°), respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Distribution between the uncertainty-weighted mean B-field direction 〈θ  B 〉 σ  and outflow direction θ Out (left panel) and between the mean B-field 〈θ  B 〉 σ  and disk orientation θ Disk (right panel). In both panels, yellow stripes indicate cases where the two vectors are perpendicular to each other (67.°5 ≤ ∣θ Diff∣ ≤ 90°), while green stripes represent cases where the two vectors are aligned (∣θ Diff∣ ≤ 22.°5). Blue circles and red crosses indicate protostars with and without clear disk orientation, respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Diagram to identify the position angle of outflows.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Other: protostars without clear outflows and without 3σ polarization detection. First column: 870 μm dust polarization intensity in color scale overlaid with the redshifted and blueshifted outflow lobes (obtained from the 12CO (3–2) line), polarization segments, and dust continuum emission (Stokes I) contours. Blue contours indicate the blueshifted outflow, while red contours indicate the redshifted outflow, with counter levels set at 5 times the outflow rms × (1, 2, 4, 8, 16, 32). The magenta segments represent the polarization. The regions of polarization intensity less than 3σ have been masked. Second column: the velocity field in color scale (obtained from the C17O (3–2) line) overlaid with the B-field segments (i.e., polarization rotated by 90°) and Stokes I contours. Third column: an enlarged perspective of 1000 au of the second column. In the second and third panels, the black segments represent the B-fields. The red and blue arrows indicate the mean direction of the redshifted and blueshifted outflows, respectively. For the velocity field, regions with an S/N less than 4 have been flagged. The gray arrows in the second and third columns indicate the mean B-field directions weighted by the intensity including all the polarization segments and weighted by the uncertainty within an annular region of 400–1000 au, respectively. In all panels, the black contour levels for the Stokes I image are 10 times the rms × (1, 2, 4, 8, 16, 32, 64, 128, 256, 512). The black dotted square in the first column corresponds to a scale of 2000 au, while the black dashed and solid circles correspond to scales of 1000 and 400 au, respectively.
Paper: On the Magnetic Field Properties of Protostellar Envelopes in Orion
Authors: Bo Huang, 博 黄, Josep M. Girart, Ian W. Stephens, Manuel Fernández López, Hector G. Arce, John M. Carpenter, Paulo Cortes, Erin G. Cox, Rachel Friesen, Valentin J. M. Le Gouellec, Charles L. H. Hull, Nicole Karnath, Woojin Kwon, Zhi-Yun Li, Leslie W. Looney, S. Thomas Megeath, Philip C. Myers, Nadia M. Murillo, Jaime E. Pineda, Sarah Sadavoy, Álvaro Sánchez-Monge, Patricio Sanhueza, John J. Tobin, Qizhou Zhang, James M. Jackson, Dominique Segura-Cox
Figure caption: Starless core. Color scale indicates the total intensity.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: The first two panels from the left show the UVIT F154W and N242W band images of the LyC leakers. In the images, north is up and east is toward the left. The black dashed circles on the UVIT images represent apertures of size 1.″6 with the same centers as in the HST/F160W images on the third panel. In the HST/F160W band images, these apertures are of size 1″ and are centered about the LyC emitters. The magenta circles indicate neighboring objects. The numbers outside the apertures indicate the redshift of the respective objects close to the LyC leakers. The fourth panel shows the HST/F435W images convolved with the F154W PSF for a size comparison. Spurious sources (see Section 4) are highlighted by dashed black squares in the F154W band. We quote the magnitude (S/N) of such sources from top to bottom. On the first row in the north: 27.07 (1.88); third row in the southwest: 26.50 (2.77); fourth row in the west 26.54 (2.69); sixth row in the southeast: 27.05 (1.93); and seventh row in the southwest: 26.76 (2.38). On the extreme right are the 3D-HST spectra of the LyC leakers. The black solid curves are the original spectra after contamination and continuum subtraction. The red curves indicate the fitted models.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: Left panel: the F154W magnitude of sources detected within 10″ × 10″ field around the 10 LyC leakers by SExtractor. The spurious sources are the ones detected by SExtractor in F154W band around the LyC leakers but not having any counterpart either in HST F435W or F160W band. Middle panel: the F154W S/N histogram of the same LyC leakers and the spurious sources as in the left panel. Right panel: the S/N distribution of 1000 and 250 circular apertures placed randomly on the entire AUDFn field of ﹩28^{\prime} ﹩ diameter (solid line) and ﹩5^{\prime} \times 5^{\prime} ﹩ HST-covered patch (dashed line) respectively, after segmenting the detected sources. Both histograms (in the right panel) show apertures only with positive flux values. All magnitudes and S/Ns are calculated based on aperture of radius = 1.″6 unless mentioned otherwise.
Paper: How to Turn Jets into Cylinders near Supermassive Black Holes in 3D General Relativistic Magnetohydrodynamic Simulations
Authors: Valeriia Rohoza, Aretaios Lalakos, Max Paik, Koushik Chatterjee, Matthew Liska, Alexander Tchekhovskoy, Ore Gottlieb
Figure caption: As time progresses, disk winds grow stronger, and the jet in model M5C transitions from a quasi-conical (R ∝ r 1) to a quasi-parabolic (R ∝ r 0.5) shape near the BH but remains quasi-cylindrical (R ∝ r 0) at r ≳ 700r g, well inside the Bondi radius. Panels (a)–(d) show density slices in the xz-plane at 20k ≤ t ≤ 50k every Δt = 10k. During this time period, the disk progressively shrinks as it thermally collapses toward the midplane due to cooling. Panel (a) shows that this opens up the space for jet sideways expansion; this also allows the backflows to come closer to the jet base and turn the jet into a cylinder. However, panels (b)–(d) show that the wind launched from the disk eventually becomes more prominent, opposes the backflows, and strongly collimates the jet. Panel (e) shows the jet radial profile at different times (see legend; we define the jet using the μ ≥ 3 condition; see text for details). The solid lines show the profile of the jet radius, averaged over Δt = 2k, at the times indicated in the legend; the shaded regions indicate one standard deviation. Panel (a) shows that at t = 20k, the jet expands conically before turning into a cylinder at r ≳ 300r g. However, panels (b) and (c) show that at t = 30k and 40k, the jet becomes quasi-conical near the BH because the jet power remains approximately constant, but the wind power increases in time. Panel (d) shows that t = 50k, the jet assumes a quasi-parabolic shape. Interestingly, throughout the simulation, the jet profile remains robustly quasi-cylindrical at r ≳ 700r g, i.e., well inside the Bondi radius. At even later times, t ≳ 60k, the jet becomes unstable (not shown).
Paper: How to Turn Jets into Cylinders near Supermassive Black Holes in 3D General Relativistic Magnetohydrodynamic Simulations
Authors: Valeriia Rohoza, Aretaios Lalakos, Max Paik, Koushik Chatterjee, Matthew Liska, Alexander Tchekhovskoy, Ore Gottlieb
Figure caption: A constant ambient medium collimates the jets, which become cylindrical, with a higher density resulting in stronger collimation and narrower jets; surprisingly, the disk cooling allows the jets to become cylindrical closer to the BH. Movies of M5 and M5C are available here (see footnote 9). Panels show 2D density slices in the xz-plane at t = 20k with each column corresponding to a different simulation. The top row is a zoom-out to show the full structure of the cocoon. The Bondi radius is shown with a dotted circle; note that each simulation has a different spatial scale. Panels (a), (c), and (e) show that as ρ amb increases, the jet propagates more slowly and becomes visually less stable. In panel (a), where ρ amb is lower, the cocoon is less prominent because the jet is stronger with respect to the ambient medium, and the jet creates a weaker shock. The jet interaction with the ambient medium redirects the material from the jet head and creates backflows, the low-density regions separated from the jet by denser disk winds as seen in panels (a), (c), (e), and (g). The backflows are the most prominent in the highest-density simulations (e) and (g), since it is harder for the jet to drill through the ambient medium. The disk cooling causes the jet to become weaker and more prone to instabilities, and panel (g) shows that the jet appears even less stable. The bottom row is a zoom-in between z = 0r g and 4000r g; the white dashed lines show jet boundaries defined as μ ≥ 5 for model M6 and μ ≥ 4 for models M7, M5, and M5C (see Section 2.2). Despite the difference in the large-scale jet morphology between models M7, M6, and M5 at r ≃ 3000r g, panels (b), (d), and (f) show a similar jet morphology at the base, which is determined by the torus and its winds. With the cooling present, which impacts the torus, the jet in panel (h) opens up at smaller distances and appears wider. We notice that the backflows reach closer to the BH, since the disk scale height decreases due to cooling.
Paper: How to Turn Jets into Cylinders near Supermassive Black Holes in 3D General Relativistic Magnetohydrodynamic Simulations
Authors: Valeriia Rohoza, Aretaios Lalakos, Max Paik, Koushik Chatterjee, Matthew Liska, Alexander Tchekhovskoy, Ore Gottlieb
Figure caption: The disk cooling in model M5C initially allows the jets to energetically dominate the disk wind, but over time, the mass accretion rate increases, and the winds become stronger, whereas the jet power slowly decreases because it is limited by the amount of available large-scale vertical magnetic flux in the system. All quantities are measured at r = 15r g to capture the disk winds and the jet but exclude backflows. Panel (a) shows the inflow, outflow, and net mass accretion rates. Until t ≃ 30k, the mass inflow and outflow rates are comparable. At t ≳ 30k, due to cooling, the disk material comes closer to the BH, and its accretion timescale decreases. More material starts falling in while approximately the same amount of material flies out, which results in an increased inward net mass flux. In panel (b), at t ≃ 30k, the power of the wind becomes larger than the power of the jet, and the winds become more prominent. The power of the jet reaches an approximately constant value at t ≃ 15k and slowly decreases over time. Panel (c) shows the jet and wind efficiencies η j and η w. The efficiency of the jet drops drastically due to the increasing mass accretion rate, which allows us to analyze the jet shape at different jet efficiencies.
Paper: How to Turn Jets into Cylinders near Supermassive Black Holes in 3D General Relativistic Magnetohydrodynamic Simulations
Authors: Valeriia Rohoza, Aretaios Lalakos, Max Paik, Koushik Chatterjee, Matthew Liska, Alexander Tchekhovskoy, Ore Gottlieb
Figure caption: Whereas the ambient medium does not impact the power of the jet near its launching region, disk cooling makes a profound difference; it causes the mass accretion to increase continuously and the jets to become progressively weaker relative to the mass inflow. This allows us to study the dependence of the jet shape on the jet efficiency. ﹩\dot{M}﹩ and P jet are measured at r = 5r g; ΦBH is measured at the BH event horizon. Panel (a) shows that models M7, M6, and M5 reach a steady state by t ≃ 15k; the mass accretion rate ﹩\dot{M}﹩ remains constant and approximately the same across the three simulations, M7, M6, and M5, because the torus and not the ambient medium dominates the BH accretion. In our model M5C, ﹩\dot{M}﹩ flattens out at t ≃ 15k–30k and then rapidly increases at 30k ≲ t ≲ 50k. Panel (b) shows a similar smooth decline in ΦBH across models M7, M6, and M5. In contrast, ΦBH in model M5C remains constant at 10k ≲ t ≲ 40k before rising slightly at t ≃ 40k. Panel (c) shows the power of the jets, which is defined as the energy flux in highly magnetized regions where the magnetization σ > 1. The jet power is approximately the same for models M7, M6, and M5 and follows the expected trend, ﹩{P}_{\mathrm{jet}}\propto {{\rm{\Phi }}}_{\mathrm{BH}}^{2}﹩. As we see in Figures 4 and 5, at t ≳ 35k, the jet in model M5 starts to become dominated by the disk winds and disappears at t ≃ 60k. The power of the jet in model M5C starts flattening out at t ≃ 15k. The jet in model M5C is less powerful yet lives longer than the jet in model M5.
Paper: How to Turn Jets into Cylinders near Supermassive Black Holes in 3D General Relativistic Magnetohydrodynamic Simulations
Authors: Valeriia Rohoza, Aretaios Lalakos, Max Paik, Koushik Chatterjee, Matthew Liska, Alexander Tchekhovskoy, Ore Gottlieb
Figure caption: First self-consistent demonstration of the jet shape transition from parabolic to conical to cylindrical in GRMHD simulations (models M7, M6, and M5) at the largest to date Bondi-to-gravitational radius scale separation of 3 orders of magnitude. The disk cooling in model M5C causes the jet to start out conical and transition to a cylindrical shape with ﹩{R}_{\mathrm{jet}}\simeq \left(100\mbox{--}200\right)\ {r}_{{\rm{g}}}﹩ well inside the Bondi radius, already at a distance of r ≃ 300r g. The M5C jet radius approximately matches the observed values for the 3C 84 jet, where ﹩{R}_{\mathrm{jet}}^{3{\rm{C}}\ 84}\gtrsim 250\ {r}_{{\rm{g}}}﹩ at r 3C 84 ≳ 350r g (Giovannini et al. 2018). This figure shows the collimation profile of the jet as a function of the distance along the jet at t = 20k when the measured ﹩\dot{M}﹩ values are similar and the P jet values are within a factor of 2 between model M5C and the rest of the models (M7–M5). Jets in models M7, M6, and M5 have a similar parabolic collimation profile extending out to r ≃ 200r g, beyond which they expand conically. Outside of the sphere of the BH gravitational influence, r ≳ r B, the jets in models M7, M6, and M5 become cylindrical; as we increase the ambient medium density, the transition point moves inward. The jet in model M5C initially expands conically up to around 300r g and then becomes nearly cylindrical.