adsabs/AstroCLIMB huggingface dataset:
Paper: Neural Networks as Surrogate Solvers for Time-dependent Accretion Disk Dynamics
Authors: Shunyuan Mao, Weiqi Wang, Sifan Wang, Ruobing Dong, Lu Lu, Kwang Moo Yi, Paris Perdikaris, Andrea Isella, Sébastien Fabbro, Lile Wang
Figure caption: Comparison of radial velocity fields from FARGO3D and PINN for a secondary with M2/M1 = 10−3 in a disk with aspect ratio h = 0.1 in Section 4.2. The PINN solution shows a smoother velocity field near the inner boundary (r = 0.4r2), while FARGO3D exhibits artificial wave reflections despite damping conditions.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: (a) The C17O(J = 3 → 2) moment 0 map imaged using robust = 1 is superposed with the contours from the dust continuum emission at levels of 1.5, 3, 7, 10, 15, 28.7, 54.9, 81.1, 110, 130, 160, 190, 210, 240, 260, 290, 320, and 340 mJy beam−1. The moment maps were produced considering pixels between 15 mJy beam−1 and the peak emission in C17O and channels between 8.4 and 9.3 km s−1. (b) Same as panel (a) but for the moment 1 velocity field map. The dust continuum contours are superposed using the same map and levels. Note that the Vlsr = 7.36  km s−1 is indicated at the color bar in each moment 1 map. (c) In this panel, we show the moment 0 map from C18O(J = 2 → 1) emission. Superposed on the map, we show the same contours from dust emission as in panel (a). The C18O moment maps were produced under the same threshold as the C17O maps and within a velocity range of 6.75–10 km s−1. (d) Same as panel (c) but for the C18O moment 1 map. The relative size of the beam is shown as a blue ellipse in the bottom left corner, and the scale is shown in the bottom right corner in each panel.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Upper panel: in color scale, we show the AM map between the inferred magnetic field and the total intensity gradient orientation. Superposed is the magnetic field morphology onto the plane of the sky as white pseudovectors plotted every 5 pixels, which is approximately Nyquist sampling. In contours, we show the continuum emission with levels following Figure 5. Lower panel: same as the upper panel, but here we show the AM map between the field and the velocity gradient orientation. The size of the beam is shown as a blue ellipse in the bottom left corner, and the scale is shown at the bottom right corner in each panel.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: DCN(J = 3 → 2) moment 0 map integrated from 7.6 to 10.3 km s−1. Overlaid are dust continuum contours at levels of 3, 10, 28, 81, 130, 190, 240, and 290 mJy beam−1 (robust = 0.5). The inferred magnetic field morphology is shown as white pseudovectors. DCN spectra from selected regions along the streamer are displayed in zoomed-in panels, with the corresponding Gaussian fits indicated by dotted red curves.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Channel maps of DCN emission shown in color scale between 7.6 and 10.3 km s−1, also following Figure 4. Superposed are DCN emission contours in black with values of 4, 9, 19, 29, 39, 49, 59, 69, 80, 90, and 100 mJy beam−1. At each channel, we also show the inferred magnetic field morphology from polarized dust emission as a map of white pseudovectors, plotted every 8 pixels to allow clearer comparison with the underlying DCN emission. The data were imaged using robust = 2 and smoothed using a kernel of ﹩0\mathop{.}\limits^{^{\prime\prime} }1﹩ to enhance the streamer.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: The Alfvén Mach number from the SVS 13A magnetic field map is shown in a color scale. The color white represents the trans-Alfvénic value of ﹩{{ \mathcal M }}_{{\rm{A}}}=1﹩, while red indicates the sub-Alfvénic regime. The magnetic field morphology is superposed as white pseudovectors plotted every 5 pixels. The map was produced from the data imaged using robust = 1. The beam is depicted as a blue ellipse in the bottom left corner, and the scale is displayed in the bottom right corner.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Channel maps of C17O emission in color scale between 5.8 and 12.7 km s−1 with the channel velocity indicated in white at the top right corner within each channel map. Superposed are C17O contours in black with values of 4.32, 19.1, 33.8, 48.6, 63.4, 78.1, 92.9, 110, 120, 140, 150, 170, 180, 200, 210, 230, 240, 260, and 270 mJy beam−1. The beam is represented as a blue ellipse in the bottom left corner, and the scale is shown in the bottom right corner.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Left panel: the histogram of the AM parameter between the total intensity gradient orientation and the magnetic field is shown as a probability density. Right panel: same as the left panel, but here we show the AM parameter between the velocity gradient orientation and the magnetic field.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: The moment 1 map from DCN emission using the same layout as Figure 8 with the SVS 13A systemic velocity indicated in the color bar (Vlsr = 7.36  km s−1). The beam is depicted as a blue ellipse in the bottom left corner, and the scale is displayed in the bottom right corner.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Channel maps of C18O emission shown in color scale between 6.7 and 8.7 km s−1, where the layout follows Figure 4. Superposed are C18O contours in black with values of 10, 30, 50, and 70 mJy beam−1.
Paper: Population-dependent r-process Scatter in the Globular Cluster M15
Authors: Lauren E. Henderson, Roman Gerasimov, Evan N. Kirby
Figure caption: Select Mg and neutron-capture element absorption lines for the star 55914 in M15. The relevant lines in each panel are highlighted in yellow. The pink spectrum is the best-fit model spectrum. The blue model spectrum has the same best-fit stellar parameters but arbitrarily low abundances of the relevant elements.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Upper panel: the polarization position angle map from the SVS 13A polarized dust continuum emission as white pseudovectors. In color scale, we show the polarized intensity emission imaged using robust = 0.5, and in contours, we show the total intensity dust continuum imaged with robust = −2 and using levels of 10, 15, 28.7, 54.9, 81.1, 110, 130, 160, 190, 210, 240, and 260 mJy beam−1. The blue oval indicates the beam obtained by imaging the data with robust = 0.5. The blue segmented lines indicate the region where the polarization position angle appears to follow the spiral substructure seen in the dust emission. Lower panel: following the upper panel, the inferred magnetic field morphology map is shown under the assumption of grain alignment by magnetic fields (i.e., pseudovectors rotated by 90°). The blue segmented line indicates the region where the inferred magnetic field lines appear to bifurcate.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Dust continuum emission maps from the SVS 13A data shown in color scale. The data were imaged using a robust weight parameter of −0.5 to highlight the resolved VLA 4 binary system and nearby sources, which are indicated by the labels. The relative size of the beam is indicated as a blue ellipse in the bottom left corner of the map, and a scale bar corresponding to 100 au length is indicated in the bottom right corner of the map.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: The polarization map of SVS 13A is shown in gray scale using robust = 0.5. The fractional polarization is shown as a pseudovector map, where each pseudovector color indicates a fractional polarization level, indicated by the color bar. The beam is shown as a blue ellipse in the bottom left corner, and the scale is highlighted in the bottom right corner.
Paper: Population-dependent r-process Scatter in the Globular Cluster M15
Authors: Lauren E. Henderson, Roman Gerasimov, Evan N. Kirby
Figure caption: Neutron-capture abundances in M15 with error <0.4 dex. The data are colored by population, with the split between populations 1 and 2 at [Mg/Fe] = 0.28 marked by the gray dashed line. Measurements with either upper or lower asymmetric error > 0.1 are less opaque.
Paper: Population-dependent r-process Scatter in the Globular Cluster M15
Authors: Lauren E. Henderson, Roman Gerasimov, Evan N. Kirby
Figure caption: [Mg/Fe] vs. [Fe/H] for stars in M15. The points are colored according to the k-means clustering. The dashed gray line marks [Mg/Fe] = 0.28, which we use to separate the stars into populations for calculating mean and dispersion.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: The Alfvén Mach number from the SVS 13A magnetic field map is shown in the color scale. Here, the color white represents the trans-Alfvénic value of ﹩{{ \mathcal M }}_{{\rm{A}}}=1﹩, while red indicates the sub-Alfvénic regime. In this case, the map was produced using a moving window of ﹩0\mathop{.}\limits^{^{\prime\prime} }5﹩ with an associated error of 10°. The magnetic field morphology is superposed as white pseudovectors plotted every 5 pixels. The map was produced from the data imaged using robust = 1. The beam is shown as a blue ellipse in the bottom left corner, and the scale is shown in the bottom right corner of the map.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Left panel: the dust emission map shown with robust = 0.5 in color scale and contours using the same levels used in Figure 1. Superposed in white pseudovectors is the intensity gradient. Also, superposed in magenta pseudovectors is the inferred magnetic field derived from the polarized emission, also imaged using robust = 0.5. Right panel: same as the left panel but with the polarization position angle as black pseudovectors. The beam is depicted as a blue ellipse in the bottom left corner, and the scale is displayed in the bottom right corner of each panel.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Left panel: the C18O moment 1 map shown with robust = 0.5 in color scale, where the velocities are relative to vlsr = 7.36 km s−1. Superposed in yellow pseudovectors is the velocity gradient, which was computed over the moment 1 map. Also, superposed in magenta pseudovectors is the inferred magnetic field as derived from the polarized emission, also imaged using robust = 0.5. In contours, we show the total intensity of the continuum emission. Right panel: same as the left panel but with the polarization position angle as black pseudovectors. The beam is depicted as a blue ellipse in the bottom left corner, and the scale is displayed in the bottom right corner of each panel.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: A comparison is shown between the polarization position angle map, as black pseudovectors, and the radiation field model, indicated by white pseudovectors. In contours and color scale, we show the total intensity of dust emission. The beam is shown as a blue ellipse in the bottom left corner, and the scale is shown in the bottom right corner of the map.
Paper: First Results from ALPPS: A Sub-Alfvénic Streamer in SVS 13A
Authors: P. C. Cortés, J. E. Pineda, T.-H. Hsieh, J. J. Tobin, P. Saha, J. M. Girart, V. J. M. Le Gouellec, I. W. Stephens, L. W. Looney, E. Koumpia, M. T. Valdivia-Mena, L. Cacciapuoti, C. Gieser, S. S. R. Offner, P. Caselli, P. Sanhueza, D. Segura-Cox, M. Fernández-López, K. Morii, B. Huang, F. O. Alves, Q. Zhang, W. Kwon, C. L. H. Hull, Z.-Y. Li
Figure caption: Left panel: the histogram of absolute angle differences between the intensity gradient orientation and the magnetic field is shown here as the probability density. Right panel: same as the left panel but for the velocity gradient orientation and the magnetic field.
Paper: Characterization of Two Cool Galaxy Outflow Candidates Using Mid-infrared Emission from Polycyclic Aromatic Hydrocarbons
Authors: Jessica Sutter, Karin Sandstrom, Ryan Chown, Oleg Egorov, Adam K. Leroy, Jérémy Chastenet, Alberto D. Bolatto, Thomas G. Williams, Daniel A. Dale, Amirnezam Amiri, Médéric Boquien, Yixian Cao, Simthembile Dlamini, Éric Emsellem, Hsi-An Pan, Debosmita Pathak, Hwihyun Kim, Ralf S. Klessen, Hannah Koziol, Erik Rosolowsky, Sumit K. Sarbadhicary, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Tony Weinbeck
Figure caption: Multiwavelength images of NGC 4424. In each panel, the white arrow represents the direction toward M87, and the dashed black contour outlines areas where the SFR surface density exceeds 0.1 M⊙ yr−1 kpc−2; i.e., the Heckman number (T. M. Heckman 2002). The H I tail extends in the opposite direction as M87, opposite the white arrow, but is outside the field of view of these images so is not shown here. Solid black contours represent areas identified as outflows and used to estimate the outflow rates in Section 4.2. In all panels, north is up and east is to the right. Top row, left to right: F770WSS, highlighting MIR PAH emission; F300M, showing the stellar disk; F770WPAH/F300M, emphasizing the differences between the stellar disk and the extended PAH emission; and F335M, showing the lack of enhanced emission from small PAHs. Bottom row, left to right: F2100W, showing the emission from larger dust grains; SFR measured by extinction-corrected Hα from MUSE; CO (2–1) integrated intensity from ALMA; and F187N map, showing the lack of Paschen α emission in outflows. The MUSE coverage is incomplete, so only the area of the galaxy with coverage is shown.
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: Voyager 1 magnetic field and plasma observations from 2004 to the end of 2024, including the magnetic field magnitude, components, azimuthal angle (λ), elevation angle (δ), and electron density ne. The red vertical lines indicate the crossing of the TS and HP. The two interstellar shocks (“sh1” and “sh2”), two pressure fronts (“pf1” and “pf2”), and the magnetic hump are denoted by the black dashed lines.
Paper: Characterization of Two Cool Galaxy Outflow Candidates Using Mid-infrared Emission from Polycyclic Aromatic Hydrocarbons
Authors: Jessica Sutter, Karin Sandstrom, Ryan Chown, Oleg Egorov, Adam K. Leroy, Jérémy Chastenet, Alberto D. Bolatto, Thomas G. Williams, Daniel A. Dale, Amirnezam Amiri, Médéric Boquien, Yixian Cao, Simthembile Dlamini, Éric Emsellem, Hsi-An Pan, Debosmita Pathak, Hwihyun Kim, Ralf S. Klessen, Hannah Koziol, Erik Rosolowsky, Sumit K. Sarbadhicary, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Tony Weinbeck
Figure caption: Top row: profiles of the median flux normalized to the central value, shown in the direction along the minor axis across the full image. The left panel shows the F770WSS data, the middle panel shows F300M tracing the stars, and the right panel shows the ratio of the two. The two outflow candidates are shown in red (NGC 4424) and yellow (NGC 4694), while two comparison galaxies of similar mass and inclination, IC 1954 and NGC 4298, are shown in green and blue, respectively. All 18 galaxies in the PHANGS sample with inclinations greater than 55° are also shown as gray lines, with the median of this comparison sample shown as a black line. Middle row: MIRI F770WSS, NIRCam F300M, and the ratio of the two maps of the primary comparison galaxy IC 1954 on the same scales as Figures 2 and 3. Bottom row: same as previous, for comparison galaxy NGC 4298. For both comparison galaxies, the PAH emission (measured in F770WSS) and starlight (measured by F300M) basically trace the same structures.
Paper: Characterization of Two Cool Galaxy Outflow Candidates Using Mid-infrared Emission from Polycyclic Aromatic Hydrocarbons
Authors: Jessica Sutter, Karin Sandstrom, Ryan Chown, Oleg Egorov, Adam K. Leroy, Jérémy Chastenet, Alberto D. Bolatto, Thomas G. Williams, Daniel A. Dale, Amirnezam Amiri, Médéric Boquien, Yixian Cao, Simthembile Dlamini, Éric Emsellem, Hsi-An Pan, Debosmita Pathak, Hwihyun Kim, Ralf S. Klessen, Hannah Koziol, Erik Rosolowsky, Sumit K. Sarbadhicary, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Tony Weinbeck
Figure caption: Same as Figure 2, but for NGC 4694. Similarly, emission in the MIR tracing dust is extended off the stellar plane. Similar to NGC 4424, the H I tail extends in the opposite direction as the arrow pointing toward M87 but is outside of the field of view of these images.
Paper: Characterization of Two Cool Galaxy Outflow Candidates Using Mid-infrared Emission from Polycyclic Aromatic Hydrocarbons
Authors: Jessica Sutter, Karin Sandstrom, Ryan Chown, Oleg Egorov, Adam K. Leroy, Jérémy Chastenet, Alberto D. Bolatto, Thomas G. Williams, Daniel A. Dale, Amirnezam Amiri, Médéric Boquien, Yixian Cao, Simthembile Dlamini, Éric Emsellem, Hsi-An Pan, Debosmita Pathak, Hwihyun Kim, Ralf S. Klessen, Hannah Koziol, Erik Rosolowsky, Sumit K. Sarbadhicary, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Tony Weinbeck
Figure caption: Three-color images of the two outflow candidate galaxies, NGC 4424 (left) and NGC 4694 (right). In both, red is F770W (PAH emission), green is F335M (stellar + PAH emission), and blue is F300M (stellar emission). Cyan contours represent the 10 MJy sr−1 and 2 MJy sr−1 in F300M, highlighting the location and extent of the stellar disk. The grayscale bar in the lower left of each image shows 1 kpc. North is up, and east is to the right in both images.
Paper: Magnetic Turbulence Intermittency and Compressibility in the Inner Heliosheath and Very Local Interstellar Medium
Authors: L.-L. Zhao, V. Florinski, G. P. Zank, M. Opher, J. Richardson, W. S. Kurth, A. Silwal, X. Zhu, N. S. M. Subashchandar, J. G. Alonso Guzman, Z. Jin
Figure caption: Scale-dependent flatness (kurtosis) of magnetic field fluctuations in the inner heliosheath and VLISM. The panels from top to bottom correspond to timescales of 3, 24, and 100 hr, respectively. The horizontal dashed–dotted line at flatness = 3 marks the Gaussian reference level.