adsabs/AstroCLIMB huggingface dataset:
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Top: the TESS light curves in 2019 and 2021. Contemporaneous ASAS-SN g-band light curves are also plotted with an offset. For the clarity of display, g-band photometry taken within 1 day is binned as one, and TESS light curves are binned to a 10-minute cadence. Bottom: the Lomb–Scargle periodogram for TESS during two sectors (each ∼24 days) and ASAS-SN g-band light curves in 2019–2020 and 2021–2022.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The relations of excess emission due to accretion in the U, B, g, and V bands, derived from photometry and spectroscopy. Open black and blue dots represent the excess emissions measured from the 2022 in-burst and post-burst light curves, respectively. The gray line represents the best-fit linear model to the 2022 burst excess emission measurements. For comparison, we also add excess emission measurements during the 2008 outburst from photometry (yellow, Juhász et al. 2012) and spectrum (green, Aspin et al. 2010), and during the quiescent state from X-Shooter spectrum (red, Figure 2).
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The relations between NEOWISE W1 photometry and mass accretion rates ﹩{\dot{M}}_{\mathrm{acc}}﹩. The median mass accretion rates are derived from ASAS-SN g (blue) and V (red) band photometry taken within 4 days apart from the NEOWISE observation epochs, and the error bars are the variability range of mass accretion rates in the 8-day time bins. The filled areas are the extrapolation ranges of our excess emission relations for g and V fluxes.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Left: the ASAS-SN g and AAVSO multicolor light curves of 2022 burst. The light curves are offset with different values for clarity. Right: Lomb–Scargle periodogram of post-burst (after MJD = 59725.0) light curves, the color scheme is the same as the left plot. The 7.417 days periodicity discovered in radial velocity measurements is also indicated (Kóspál et al. 2014).(The data used to create this figure are available.)
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Phase-folded post-burst light curves in the UBVRI and g bands from AAVSO. The multicolor light curves are phase-folded with P = 7.385 days and to the U-band best-fit reference date JD = 2459716.96. The red vertical lines indicate the location of brightness maxima for different wavelengths to show the phase lags. The blue error bar at the lower left of each panel shows the median photometric errors in each band.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The phase-folded light curves of ASAS-SN V band (red), g-band (blue), and TESS (black) light curves, all folded to P = 7.42 days and JD = 2457200.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Top: the ASAS-SN g and NEOWISE W1/W2 photometry before and after the 2022 burst. Bottom: the CMD of W1 and W1/W2. The color trend predicted by the extinction of A  V  = 4 mag is indicated by a black arrow.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The histograms of mass accretion rates measured from the excess U-, B-, ASAS-SN g-, and V-band emission in the post-burst light curves of the 2022 burst. Gaussian fits of the ﹩\mathrm{log}{\dot{M}}_{\mathrm{acc}}﹩ histograms are plotted with red dashed lines.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Near-IR light-curve models for the progenitor candidate of SN 2023ixf constructed using the power spectrum on the left, which is recovered from the Spitzer data (Figure 5 left) scaled by a factor 2.2 to account for the larger variability amplitude in the near-IR (Figure 4). The shaded regions indicate the 1σ confidence intervals for the models. Despite the scarce data points, the light curves look reasonable as compared to those built using various modified versions of the power spectrum shown in Figures 8–10.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Left: reconstructed power spectrum of the Spitzer 3.6 μm light curve with its 99% confidence interval highlighted by the gray shaded region. The gray dotted line marks the location of the identified period. Right: reconstructed light curves using the power spectrum on the left for the Spitzer 3.6 and 4.5 μm data shown by the blue and red curves, respectively. The shaded colored regions mark their 1σ confidence intervals.
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: Galaxies belonging to each of the four subsamples. We present examples for each group and show their χ 2 and IRAC-1 cutouts, on which we superimposed the radio (solid lines) and the χ 2 and IRAC-1 (dashed lines) contours at 3σ, 4σ, and 5σ (crimson). From the upper left: (a) Type 0: galaxies with no counterparts up to MIPS 24 μm; (b) Type 1: isolated galaxies in all bands and with a counterpart in the MIR filters; (c)Type 2: galaxies having a counterpart and a nearby contaminant in one or more bands; (d) Type 3: like Type 0, but close to another radio source with a counterpart in one or more bands.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Modified form of the power spectrum recovered from the Spitzer data (left, see Section 3) and the near-IR light-curve models for the progenitor candidate of SN 2023ixf constructed using it (right). The gray curve in the left panel shows the original power spectrum, while the shaded regions in the right panel indicate the 1σ confidence intervals for the light-curve models. Here the modified power spectrum is obtained by interpolating across the power peak and scaling it to conserve the total power.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: H-R diagram based on the BPASS single-star evolutionary tracks. Different colors indicate different initial masses of the models as indicated in the legend (in M ⊙). The gray shaded parallelogram around the ★ symbol shows the possible location of the progenitor candidate of SN 2023ixf, assuming a late M-type supergiant with T eff ranging from 3200 to 3500 K (see text). The vertical width of the region corresponds to the uncertainty in ﹩\mathrm{log}(L/{L}_{\odot })﹩ at a given temperature. The faint gray crosses mark the locations of cool and luminous (﹩\mathrm{log}(L/{L}_{\odot })\gt 4.7﹩), directly detected progenitors of previous SNe-IIP/II-L from Smartt (2015) and Van Dyk (2017).
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Similar to Figure 8. Here the modified power spectrum is obtained by fitting a power law to the original spectrum from the Spitzer data, adding a peak at some higher frequency (which is not a harmonic of the original peak frequency), and scaling the resulting spectrum to conserve the total power. The flattening at the lowest frequency is due to extrapolation using the nearest-neighbor value.
Paper: The SN 2023ixf Progenitor in M101. I. Infrared Variability
Authors: Monika D. Soraisam, Tamás Szalai, Schuyler D. Van Dyk, Jennifer E. Andrews, Sundar Srinivasan, Sang-Hyun Chun, Thomas Matheson, Peter Scicluna, Diego A. Vasquez-Torres
Figure caption: Similar to Figure 8. Here the modified power spectrum is obtained by fitting a power law to the original spectrum from the Spitzer data and scaling it to conserve the total power. The flattening at the lowest frequency is due to extrapolation using the nearest-neighbor value.
Paper: Illuminating the Dark Side of Cosmic Star Formation. II. A Second Date with RS-NIRdark Galaxies in COSMOS
Authors: Meriem Behiri, Margherita Talia, Andrea Cimatti, Andrea Lapi, Marcella Massardi, Andrea Enia, Cristian Vignali, Matthieu Bethermin, Andreas Faisst, Fabrizio Gentile, Marika Giulietti, Carlotta Gruppioni, Francesca Pozzi, Vernesa Smolçić, Gianni Zamorani
Figure caption: Flow chart representing the selection process of the sample. The dark blue part of the chart indicates those steps made by T21, while the purple contours are used to highlight the ones made in this work.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Left: narrow passband 5007 Å image, leading to the discovery of a large, very faint [O III] emission nebula near M31. Right: negative image after blue continuum subtraction and software processing. The bright object near the top center is the 4.5 mag B5 V star HD 4727 (ν Andromeda).
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Wide-field Hα images showing faint emission around M31. Image FOVs as shown are 3.°8 × 3.°8 (top left) and 7.°1 × 7.°1 (top right). Bottom: VTSS Hα image; 15.°6 × 7.°1. North is up, east is to the left for all panels.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Deep [O III] image of the sky around M31. The FOV as shown is 9.°2 × 14.°5. North is up, east is to the left.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Close up of the 1.°5 long [O III] 5007 Å emission nebula (SDSO) located southeast of M31's nucleus.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Spatial emission details of SDSO as seen in two independent sets of deep [O III] 5007 Å images. Exposure totals were 46 hr and 110 hr for the left and right images, respectively. North is up, east is to the left.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: Matching [O III] (top) and Hα+[N II] (middle) images along with a color composite (bottom) of SDSO and its immediate surroundings. North is up, east is to the left.
Paper: The Spatial and Emission Properties of the Large [O III] Emission Nebula Near M31
Authors: Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Marcel Drechsler, Xavier Strottner, Yann Sainty, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker, Justin Rupert
Figure caption: High-contrast [O III] image showing SDSO’s maximum extent. North is up, east is to the left.
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Existence diagrams for a symmetric bi-ion plasma mixture. Existence domain of fast and slow modes of IA solitary waves vs. the streaming velocity (beam speed (U), for (a) κ  e  = 20; (b) κ  e  = 4; (c) κ  e  = 3; (d) κ  e  = 2, and for a fixed value of δ = 0.5. The fast mode is shown in blue color and the slow mode is in red. The solid curves correspond to the sonic boundary M  s , while the dashed curves correspond to M  l . The black dotted curve representing M = U separates the fast from the slow regime.
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption:  ω  F  in the k–U plane corresponding to the fast IA mode (a) for κ  e  = 20 (quasi-Maxwellian) and (b) for κ  e  = 2 (strongly nonthermal case) and for fixed δ = 0.5. Note that only ω  F  > 0 is taken into account (as ω  F  < 0 will simply be symmetric, lying on the negative axis).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Growth rate Im(ω  S ) in the k–U plane corresponding to slow IA (unstable) mode (a) for κ  e  = 20 (quasi-Maxwellian) and (b) for κ  e  = 2 (strongly nonthermal case) and for fixed δ = 0.5. Note that only ω  F  > 0 is taken into account (as ω  F  < 0 will simply be symmetric, lying on the negative axis).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Re(ω  S ) in the k–U plane corresponding to the (real part of the) slow (stable) IA mode (a) for κ  e  = 20 (quasi-Maxwellian) and (b) for κ  e  = 2 (highly superthermal regime), for a fixed value δ = 0.5. Note that only Re(ω  S  > 0) is taken into account as Re(ω  S  < 0) is symmetrical in the negative axis.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: Top: NEOWISE W1 (orange) and W2 (black) photometry. Middle: the ASAS-SN g- (red) and V-band (blue) light curves of EX Lup between 2015 and 2022, shown in blue and red dots, respectively. The bursts in 2020 and 2022 are indicated with black sticks. The two gray vertical lines indicate the epochs when two sectors of TESS observations are taken. Bottom: the Lomb–Scargle periodograms for the V-band (left) and g-band (right) light curves. The g-band light curves in 2020 and 2022 are excluded from periodogram analysis due to the presence of bursts.
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The full light curve collections of EX Lup. The photometry data covered in this paper come from DASCH (blue pentagons), AAVSO (black dots), ASAS-SN (red and blue diamonds), NEOWISE (black and orange triangles), TESS (orange squares), and SMARTS/1.3 m telescope (red and green crosses). The timestamps of several outbursts and bursts from EX Lup are also indicated in the figure.(The data used to create this figure are available.)
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The best fit (red) of EX Lup X-Shooter spectrum (black) taken on 2010 May 4. The spectrum is dereddened with A  v  = 0.1 mag, fitted with a photosphere template (blue) and a slab model (gray).
Paper: The Accretion History of EX Lup: A Century of Bursts, Outbursts, and Quiescence
Authors: Mu-Tian Wang, 牧天 王, Gregory J. Herczeg, 雷歌 沈, Hui-Gen Liu, 慧根 刘, Min Fang, 敏 房, Doug Johnstone, Ho-Gyu Lee, Frederick M. Walter, Franz-Josef Hambsch, Carlos Contreras Peña, Jeong-Eun Lee, Mervyn Millward, Andrew Pearce, Berto Monard, Lihang Zhou, 立杭 周
Figure caption: The Balmer jump (top) and U-band spectra (bottom) for EX Lup in quiescence (red) and outburst (black). The accretion spectrum of EX Lup during outburst has a bluer slope and maintains a Balmer jump. The U-band spectrum during the outburst is highly structured, indicating that the accretion flow has an optically thick photosphere. In quiescence, the U-band spectrum of EX Lup (and most other accreting young stars) is mostly featureless.
Paper: Simultaneous Observation of the Inner and Outer Electron Diffusion Region in Reconnection with Large Guide Field
Authors: Z. C. Tian, M. Zhou, H. Y. Man, Z. H. Zhong, X. H. Deng, D. J. Gershman, Y. V. Khotyaintsev, C. T. Russell
Figure caption: Successive observation of the inner and outer EDR by the four MMS spacecraft. (a)  L  component of magnetic field; (b) the magnitude of the electron bulk velocity; (c)  L  and (d)  M  component of the electron bulk velocity; (e) ﹩{\boldsymbol{J}}\cdot {{\boldsymbol{E}}}^{{\prime} }﹩; (f) ﹩{{J}_{L}E}_{L}^{{\prime} };﹩ (g) ﹩{{J}_{M}E}_{M}^{{\prime} };﹩ (h) ﹩{{E}^{{\prime} }}_{M};﹩ (i) the degree of electron nongyrotropy ﹩\ \sqrt{Q};﹩ (j) schematic view of this reconnection layer and the spacecraft trajectory in the L–N plane.
Paper: Simultaneous Observation of the Inner and Outer Electron Diffusion Region in Reconnection with Large Guide Field
Authors: Z. C. Tian, M. Zhou, H. Y. Man, Z. H. Zhong, X. H. Deng, D. J. Gershman, Y. V. Khotyaintsev, C. T. Russell
Figure caption: Overview of MMS1 observations from 22:00 to 22:25 UT on 2016 January 7. (a) The three components of magnetic fields; (b) the magnitude of the magnetic field; (c) the three components of the ion bulk velocity; (d) electron number density; (e) ion and (f) electron parallel (blue) and perpendicular (red) temperatures; (g) ion and (h) electron differential energy fluxes. The red dashed line marks the secondary reconnection event studied in this paper. The vectors are displayed in GSE coordinates.
Paper: Simultaneous Observation of the Inner and Outer Electron Diffusion Region in Reconnection with Large Guide Field
Authors: Z. C. Tian, M. Zhou, H. Y. Man, Z. H. Zhong, X. H. Deng, D. J. Gershman, Y. V. Khotyaintsev, C. T. Russell
Figure caption: Detailed observations of the secondary reconnection by MMS1 (left column) and MMS3 (right column). (a) and (f) magnetic field; (b) and (g) ion bulk velocity; (c) and (h) electron bulk velocity; (d) and (i) electric current density calculated by plasma density and velocity; (e) and (j) energy dissipation ﹩{\boldsymbol{J}}\cdot {{\boldsymbol{E}}}^{{\prime} }={\boldsymbol{J}}\cdot ({\boldsymbol{E}}+{{\boldsymbol{V}}}_{{\boldsymbol{e}}}\times {\boldsymbol{B}})﹩. All the vectors are displayed in the LMN coordinate system. The background ion flow velocity has been subtracted from the ion and electron bulk velocity.
Paper: The Inhomogeneity Effect. I. Inhomogeneous Surface and Atmosphere Accelerate Planetary Cooling
Authors: Xi Zhang
Figure caption: Planck blackbody emission with brightness temperature at a frequency of 50 THz (∼6 μm). The black dots represent the Planck emission at 200 and 800 K, and intensity at their average temperature of 500 K (black-filled dot), which is smaller than the average intensity (red-filled dot) of the 200 and 800 K emissions. The inequality arises from the convexity of the Planck function.
Paper: Evidence for Large-scale, Rapid Gas Inflows in z ∼ 2 Star-forming Disks
Authors: R. Genzel, J.-B. Jolly, D. Liu, S. H. Price, L. L. Lee, N. M. Förster Schreiber, L. J. Tacconi, R. Herrera-Camus, C. Barfety, A. Burkert, Y. Cao, R. I. Davies, A. Dekel, M. M. Lee, D. Lutz, T. Naab, R. Neri, A. Nestor Shachar, S. Pastras, C. Pulsoni, A. Renzini, K. Schuster, T. T. Shimizu, F. Stanley, A. Sternberg, H. Übler
Figure caption: Top and right: images of continuum and Hα velocity, velocity dispersion, and their residuals in GS4_43501 (z = 1.61). Bottom left: 1D Hα intensity, velocity, and velocity dispersion cuts along PAmajor, as well as the best-fit DYSMAL model (red line).