adsabs/AstroCLIMB huggingface dataset:
Paper: A Mildly Relativistic Outflow Launched Two Years after Disruption in Tidal Disruption Event AT2018hyz
Authors: Y. Cendes, E. Berger, K. D. Alexander, S. Gomez, A. Hajela, R. Chornock, T. Laskar, R. Margutti, B. Metzger, M. F. Bietenholz, D. Brethauer, M. H. Wieringa
Figure caption: Radio spectral energy distributions for our VLA data as in Figure 3, but for a two-outflow model. Here, Outflow 1 has a peak near ∼1 GHz (green lines), Outflow 2 has a peak near ∼3 GHz (orange lines), and they combine to give a total outflow (black lines).
Paper: A Mildly Relativistic Outflow Launched Two Years after Disruption in Tidal Disruption Event AT2018hyz
Authors: Y. Cendes, E. Berger, K. D. Alexander, S. Gomez, A. Hajela, R. Chornock, T. Laskar, R. Margutti, B. Metzger, M. F. Bietenholz, D. Brethauer, M. H. Wieringa
Figure caption: VLA+ALMA data at 1251–1253 days (blue points), Chandra data at 1253 days (yellow point), UVOT data at 1182 days (purple circle), and ZTF data at 1030 days (red circle). Also shown are the models from Figure 8 (dashed; no cooling break), and models that include a cooling break to match the X-ray flux density (black; Equation (7)). We find that ν  c  ≈ 1013 Hz.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Comparison of synthesized EUVIs of the model with SOHO/EIT EUVIs. The columns are, from left to right, 171, 195, and 284 Å. Top panels: observational SOHO/EIT images. Middle panels: synthesized EUVIs of the model driven by the real magnetogram. Bottom panels: synthesized EUVIs of the model driven by the synthetic magnetogram. The images are generated for CRs (a) 1925, (b) 1957, (c) 1989, (d) 2021, (e) 2069, (f) 2086, (g) 2112, (h) 2151, and (i) 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: OMNI data (black) and SWMF results for solar wind parameters driven by real (red) and synthetic (blue) magnetogram data for CRs (a) 1925, (b) 1957, (c) 1989, (d) 2021, (e) 2069, (f) 2086, (g) 2112, (h) 2151, and (i) 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Comparison of the distributions for solar wind at 1 au. Shown are OMNI data (black) and SWMF results for solar wind parameters driven by real (red) and synthetic (blue) magnetogram data for CRs (a) 1925, (b) 1957, (c) 1989, (d) 2021, (e) 2069, (f) 2086, (g) 2112, (h) 2151, and (i) 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Correlation between the mean values of the solar wind parameters obtained from SWMF and OMNI observations at 1 au for CRs 1925, 1957, 1989, 2021, 2069, 2086, 2112, 2151, and 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Side-by-side comparison of the real and synthetic maps for CRs that occurred in solar cycles 23 and 24.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Top: pulsing history of model A123p65. The central temperature (solid red line) and density (solid blue line) are shown as a function of time to core collapse. A weak pulse (T  p  = 2.91 GK) at 149.1 days before collapse launches a shock that unbinds most of the envelope. Two stronger, closely separated pulses at 132.8 days (T  p  = 3.05 GK) and 130.3 days (T  p  = 3.46 GK) illuminate the previously ejected material. Finally, a series of three rapid pulses of 0.977, 0.958, and 0.925 days (T  p  = 4.04, 4.25, and 4.86 GK) lead to a terminal brightening just as the core collapses to a black hole (the brightening is delayed from the time of pulses because of diffusion time). Middle: comparison of the bolometric light curve of model A123p65 with that estimated for SN 1961V. Time is plotted relative to the observed peak for SN 1961V on the bottom axis and to core collapse on the top axis. The single observed point at –366 days is omitted in this plot, as are observations beyond 700 days post-peak. Bottom: radiation transport in model A123p65. The velocity (red) and luminosity (blue) are shown as a function of mass for three different times, 10 days (solid), 20 days (dashed), and 25 days (dashed–dotted) after core collapse (see the timescale on the top of the middle panel). Note the diffusion of light ahead of the shock. Asterisks indicate the location of the electron scattering photosphere.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Comparison of the bolometric light curves of models TH109p25 and A126p65 with observations of SN 1961V. The model luminosities have a complex structure resulting from both repeated explosions and shell collisions. The models predict bright prior events that might have escaped detection. Note that days −260 to −165 and −625 to −530 relative to peak (vertical gold bands) are when SN 1961V is not observable owing to R.A. constraints (Section 5.4). Upper bounds on the luminosity at −453 and −476 days before peak can be problematic depending on the spectrum and exact timing of pulses. At time zero on the top axis the core collapses to a black hole and is removed from the calculation. Very late time emission might be augmented by interaction with a pre-SN stellar wind.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Top: bolometric light curves of models TH93p25, TH95p25, TH97p25, TH99p25, TH102p25, and TH103p25 (Table 3). In all cases, the duration of pulsing activity is shorter than that of the initial plateau in the light curve. Multiple shocks from the pulses deposit energy in the deep interior that diffuses, in waves, to the photosphere. The greater the mass of the star, the longer this pulsing persists. Later sharp structure in some of the light curve is introduced by fast-moving thin shells that eventually catch up with slower ones after core collapse. Bottom: light curves for a similar set of models, M105p9, M106p9, M107p9, M108p85, and M109p85, with smaller radii and denser hydrogen envelopes. The initial masses are smaller because of the reduced mass-loss rates associated with the smaller radii. The light curves are similar to those for the “TH” models, except at early times when the smaller radius causes the emission to be fainter.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Early bolometric light curves of models TH114p25 and TH115p25 compared with SN 1961V for the 4.5 yr when the SN was well observed. Time for the model is measured since the first pulse (top axis) and for the SN relative to the time of its observed peak luminosity (bottom axis). The model luminosity prior to t = 0 is the pre-SN star. Emission after about 500 days is from the residual stars, both of which retain a mass at this point of 50 M ⊙. The overall light curve of SN 1961V is in good agreement with this model, though not the initial observed point at −366 days, which must have other causes. In model TH115p25, a stellar remnant would still be shining at approximately the Eddington luminosity (∼1040 erg s−1) today, but for model TH114p25 the star died around 2001.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Velocity (black line) and ejected H/He composition for model A123p65 as a function of mass. The velocities at the time of iron core collapse (solid line) and at 700 days (dashed line) are shown. The photosphere is just outside of the high-velocity material in the pre-SN star. Velocities in the hydrogen-rich material range from 1500 to 2100 km s−1, except for a small amount of high-velocity material (∼3000 km s−1) at the outer edge. The plot for model A123p7 would be similar, but the final velocities are about 15% greater.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Top: pulsing history of model TH115p25 during the first series of pulses. Additional events occurred 106 yr later, culminating in the collapse of the core to a black hole. Central temperature (solid red line) and density (dashed blue line) are plotted vs. time since the first pulse. The first pulse ejected the hydrogen envelope, producing a low-energy SN II-P. The second pulse ejected matter that interacted with the prior ejecta to produce the late peak in the light curve. Bottom: the velocity and composition profile for model TH115p25 at a time just before peak (solid line) and much later when the luminosity has declined to 1041 erg s−1. The high velocities at the earlier time are well beneath the photosphere.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Terminal velocities (top) and effective emission temperature histories (bottom) of models TH93p25, TH95p25, TH97p25, TH99p25, TH102C, and TH103p25 during a time when the electron scattering photosphere is well defined. Lower-mass explosions resemble typical Type II-P SNe, albeit with a low energy-to-mass ratio. The higher-mass models show distinctive signatures of pulsationally generated shock heating. At late times all the ejected matter ends up coasting at the same speed. This is probably an artifact of the 1D calculation. During a pulse, the luminosity increases at nearly constant radius, so the temperature rises.
Paper: SN 1961V: A Pulsational Pair-instability Supernova
Authors: S. E. Woosley, Nathan Smith
Figure caption: Top: the pulse history for A123p65 shows three pulses plus a final collapse to a black hole. Temperature is the solid red line, and density is the dashed blue line. Bottom: ejected composition and velocity for the same model. The solid line shows the velocity at the time of core collapse with high values due to the terminal pulses shown in the top panel. The dashed line shows the velocity years later at the last point plotted in Figure 10.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Top: spectral index (α mm for ﹩{S}_{\nu ,\mathrm{mm}}^{\mathrm{peak}}\propto {\nu }^{-{\alpha }_{\mathrm{mm}}}﹩) against detection significance for the AGNs that were observed with more than two spectral windows and whose nuclear emission was significantly detected in all windows. The orange line indicates α mm = −3.5, expected for thermal emission (modified blackbody emission) from dust. Bottom: the statistical error of the mm-wave spectral index as a function of detection significance. Blue data points indicate objects observed with spectral windows covering 14 GHz ∼ 18 GHz, while NGC 1068 and NGC 1194 (orange) were observed with narrower bandwidths (3 GHz ∼4 GHz). A fitted line to all objects, except NGC 1068 and NGC 1194, is indicated by the dashed line and is expressed as ﹩\mathrm{log}{\alpha }_{\mathrm{mm}}^{{\rm{e}},\mathrm{stat}}=1.53-1.03\times \mathrm{log}({S}_{\nu ,\mathrm{mm}}^{\mathrm{peak}}/{\sigma }_{\mathrm{mm}})﹩.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: ALMA 600 pc × 600 pc Band-6 images for NGC 985, MCG −1−24−12, and NGC 3393 obtained with beams (left bottom corners) of ≈100 pc, a typical resolution achieved in our sample (Figure 3). The numbers to the left of the object names are the numbers assigned in this study (Table A1) and Paper II. The indicated frequency in the figure is the rest-frame central frequency of the collapsed spectral window adopted, after removing any strong emission line flux. Each central black cross indicates the peak of the nuclear mm-wave emission, expected to be the AGN position. C, CE, and CB are morphological parameters assigned. C, E, and B indicate nuclear core emission, extended emission visually connected to the core component, and a blob (or blobs) separated from the core, respectively. Colors are assigned according to flux density in units of Jy beam−1 following the color bar on the right side. The orange contours indicate where flux densities are 5σ mm, 10σ mm, 20σ mm, 40σ mm, 80σ mm, and 160σ mm. For NGC 985, MCG −1−24−12, and NGC 3393, σ mm = 0.02 mJy beam−1, σ mm = 0.01 mJy beam−1, and σ mm = 0.02 mJy beam−1, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption:  Mm-wave luminosity vs. 2–10 keV, 12 μm, and bolometric luminosities. The 12 μm luminosities take into account only an AGN component determined by the SED analysis of Ichikawa et al. (2019). AGNs with upper limits are shown as black circles. The black dashed lines indicate the best-fit linear regression lines, and the gray regions denote the ±1σ scat ranges.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Correlation of mm-wave and 14–150 keV luminosities, derived by using ALMA and BAT, respectively. AGNs with upper limits are shown as black circles. The black dashed line indicates the best-fit linear regression line, while the gray region denotes the ±1σ scat range.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Ratio of the flux density (﹩{S}_{\nu ,\mathrm{mm}}^{250\,\mathrm{pc}}﹩) measured by an aperture with a diameter of 250 pc and the peak one as a function of the spatial resolution achieved. Values below ∼1 particularly in a range ﹩{\theta }_{\mathrm{beam}}^{\mathrm{ave}}\gt 150﹩ pc are just due to the prescription to calculate the aperture flux density (see the text).
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption:  Mm-wave-to-X-ray luminosity ratio as a function of the physical resolution achieved in our ALMA data. AGNs with upper limits are shown as black circles. No significant correlation is found with P cor ∼ 0.19. An important point of this plot is that the slope of the regression line (dashed line) is ≈ 0.0007. Thus, the difference in the ratio is ≈0.1 dex between 200 and 10 pc. The flat slope can be interpreted as the ubiquitous presence of a compact component on a scale of ≲10 pc that is related to AGN X-ray emission.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plot of the mm-wave index and the index derived from ∼230 and 100 GHz data. The dashed line indicates the one-to-one relationship.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Histogram for the significance of peak emission. We regard emission with peak flux density less than 5σ mm as a nondetection. Among our 98 objects, significant emission was detected for 89 objects.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption:  Mm-wave luminosity vs. redshift for our sample.
Paper: The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA
Authors: Ward S. Howard, Meredith A. MacGregor, Rachel Osten, Jan Forbrich, Steven R. Cranmer, Isaiah Tristan, Alycia J. Weinberger, Allison Youngblood, Thomas Barclay, R. O. Parke Loyd, Evgenya L. Shkolnik, Andrew Zic, David J. Wilner
Figure caption: The Güdel–Benz Relation (GBR) describes the relative emission of stars in the SXR and radio, in both quiescent (panel (A)) and flaring (panel (B)) states. A departure from the GBR can indicate changes in the emission mechanism; such departures have been observed for radio-loud M-dwarfs with rotation periods >10 days (Magaudda et al. 2020) and ultracool dwarfs, reproduced here from Williams et al. (2014). We find the quiescent emission of Proxima Cen to be consistent with the GBR while the flare emission is radio-loud under the assumption of the X1.5 Krucker et al. (2013) spectral energy distribution (SED). The star's quiescent emission of 0.1 mJy at 230 GHz (MacGregor et al. 2018) is also similar to the ∼0.2 mJy observed at 1.6 GHz (black ×; Pérez-Torres et al. 2021) although this may be electron–cyclotron maser emission. Differences between flares at 5 GHz and 200 GHz are usually within a factor of ∼10 during flares, assuming an SED dominated by gyrosynchrotron emission (Krucker et al. 2013). The X1.5 SED from Krucker et al. (2013) is used to predict the 5 GHz emission of our flare with an upward error bar. The star symbol is the band 6 value and the error bar is the difference between that and the 5 GHz prediction (Krucker et al. 2013). Following Williams et al. (2014), quiescent emission is shown with colored boxes and flares (colored star shapes) are connected to their quiescent source with dashed lines. <M6.5 sources and flares are teal, while >M6.5 sources are lime green. The quiescent value of Proxima Cen is from the left-hand panel.
Paper: The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA
Authors: Ward S. Howard, Meredith A. MacGregor, Rachel Osten, Jan Forbrich, Steven R. Cranmer, Isaiah Tristan, Alycia J. Weinberger, Allison Youngblood, Thomas Barclay, R. O. Parke Loyd, Evgenya L. Shkolnik, Andrew Zic, David J. Wilner
Figure caption: Panel (A): the millimeter emission from our X1 flare analog is both much stronger in intensity and shorter in duration than a X1.5 solar flare (reproduced from Krucker et al. 2013). Note the change in the y-axis scaling to illustrate both flares. We only show the second and larger ALMA flare peak as a representative event. Panel (B): we reproduce the soft X-ray (SXR)–millimeter scaling relationship from Krucker et al. (2013) and overlay our flare in red. We extrapolate the likely position in SXR–millimeter parameter space of larger flares previously observed from M-dwarfs with ALMA by assuming the ratio of SXR and millimeter emission from our flare.
Paper: The Mouse That Squeaked: A Small Flare from Proxima Cen Observed in the Millimeter, Optical, and Soft X-Ray with Chandra and ALMA
Authors: Ward S. Howard, Meredith A. MacGregor, Rachel Osten, Jan Forbrich, Steven R. Cranmer, Isaiah Tristan, Alycia J. Weinberger, Allison Youngblood, Thomas Barclay, R. O. Parke Loyd, Evgenya L. Shkolnik, Andrew Zic, David J. Wilner
Figure caption: Equivalent widths for du Pont optical line emission on the same time axis as the Chandra flare emission but at ∼10 min observing cadence. The Chandra light curve is shown for reference. Each line but Ca II H appears to peak at the same time as the spft X-ray at this cadence. The equivalent width formal uncertainties are insignificant.
Paper: Hi-C 2.1 Observations of Reconnection Nanojets
Authors: Ritesh Patel, Vaibhav Pant
Figure caption: Relation between estimated parameters of reconnection nanojets where the outward jets are shown in red while the blue represents the inward moving ones. The correlation coefficients for the individual classes are shown in their respective colors. For the relation between length and width, negligible correlation is found for the inward directed jets.