adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: The 12CO(3−2) and 13CO(3−2) moment 0 and moment 1 maps of HD 110058 (left and middle panels, respectively). Colors show the velocity centroids for each pixel, i.e., moment 1. Contours show the integrated intensity of the line emission. The first contour is 3 times the rms noise, and each subsequent contour level increases with a step of 3 × rms (i.e., contour levels are 3, 6, 9, 12, and so on, times the rms). The corresponding rms noise for the zeroth moment of 12CO(3−2) and 13CO(3−2) is 3.4 and 4.9 mJy beam−1 km s−1, respectively. Right: radial distribution of 0.88 mm continuum, 12CO (3−2), and 13CO (3−2) obtained from spatially integrating the continuum and moment 0 images along a line perpendicular to the major axis of the disk. The profiles have been normalized to unity for comparison. The blue region shows the projection of the synthesized beam size in the direction of the disk’s major axis.
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: The 12CO (2−1) and 13CO(2−1) moment 0 and moment 1 maps of HD 110058 (left and middle panels, respectively). Colors show the velocity centroids for each pixel, i.e., moment 1. Contours show the integrated intensity of the line emission. The first contour is three times the rms noise, and each subsequent contour level increases with a step of 3 × rms (i.e., contour levels are 3, 6, 9, 12, and so on, times the rms). The corresponding rms noise for the zeroth moment is listed in Table 2. Right: radial distribution of 1.33 mm continuum, 12CO (2−1), and 13CO (2−1) obtained from spatially integrating the continuum and moment 0 images along a line perpendicular to the major axis of the disk. The profiles have been normalized to unity for comparison. The blue region shows the projection of the synthesized beam size in the direction of the disk’s major axis.
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: ALMA 1.32 and 0.88 mm continuum images of the HD 110058 disk (left and right panels). Contour levels are shown at 3, 7, 14, and 21 times the rms of each image (8 and 17 μJy beam−1, respectively). The position of the star is indicated with a black plus sign. The integrated fluxes reported in Table 2 were integrated within a circular region centered at the star position of 1.″0 in radius. The ellipse in the lower left corner represents the synthetic beam of the data.
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: Posterior distribution obtained for the disk peak radius, inner and outer FWHM, vertical aspect ratio, and inclination. The blue lines show the parameter values that give the best fit, whereas the vertical dashed lines show the 16th, 50th, and 84th percentiles. The contours represent the 68%, 95%, and 99.7% confidence levels.
Paper: Millisecond Pulsars in Dense Star Clusters: Evolution, Scaling Relations, and the Galactic-center Gamma-Ray Excess
Authors: Claire S. Ye, Giacomo Fragione
Figure caption: Same as Figure 2 but for models with a metallicity Z = 0.02 and Galactocentric distance R  g  = 20 kpc.
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: Left: Band 7 best-fit dust ring model image. Middle: Band 7 residual image after subtracting the model from the data. The color stretch ranges from −3σ to 3σ, where σ = rms of 1.7 × 10−2 mJy beam−1. Right: Band 6 residual image after subtracting the model from the data. The color stretch ranges from −3σ to 3σ, where σ = rms of 8.6 × 10−3 mJy beam−1.
Paper: ALMA Observations of the HD 110058 Debris Disk
Authors: Antonio S. Hales, Sebastián Marino, Patrick D. Sheehan, Silvio Ulloa, Sebastián Pérez, Luca Matrà, Quentin Kral, Mark Wyatt, William Dent, John Carpenter
Figure caption: Triangle plots of the posterior probability distribution function for the gas disk model that fits 12CO(3–2), 13CO(3–2), and 13CO(2–1) simultaneously. The blue lines show the point with the highest probability, i.e., the most likely model from the fit. The maximum-likelihood values and uncertainties corresponding to the range around these values including 95% of all walkers in the posterior are shown at the top of each column.
Paper: Millisecond Pulsars in Dense Star Clusters: Evolution, Scaling Relations, and the Galactic-center Gamma-Ray Excess
Authors: Claire S. Ye, Giacomo Fragione
Figure caption: Same as Figure 2 but for models with a metallicity Z = 0.02 and Galactocentric distance R  g  = 8 kpc.
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: Stellar population synthesis fits to the leaker and nonleaker spectra. The left panels show P-Cygni N V features in the leaker (top) and the nonleaker (bottom); the middle panel shows P-Cygni C IV features in the leaker (top) and the nonleaker (bottom); and the right panel shows He II 1640 features in the leaker (top) and the nonleaker (bottom). The orange line represents the best-fit light-weighted Starburst99 model: the inferred ages are 3.3 Myr for the leaker and 11.8 Myr for the nonleaker.
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: Magellan/MagE spectra showing the stacked spectra of the LyC leaking regions (blue) and the nonleaking regions (red). The leaker spectrum is normalized by a median continuum level between 1400 and 1500 Å, while the nonleaker spectrum is further offset by 0.5, for clarity of plotting. The corresponding error spectra are shown by the dotted blue line (leaker) and the dotted red line (nonleaker). The figure shows several emission (black label) and absorption (red label) features. The emission lines are more prominent in the leaker spectrum, while the absorption lines, particularly low-ionization interstellar features (see Section 3 for more details), are prominent in the nonleaker spectrum.
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: HST F814W image of the Sunburst Arc, showing the positions of the FIRE and MagE slits. The red rectangles show the positions and orientations of 10 FIRE slits, and the black rectangles show the positions and orientations of nine MagE slits. The solid and dashed rectangles indicate knots leaking and not leaking LyC photons, respectively. The numbers indicate multiple images of a LyC emitting region.
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: Magellan/FIRE spectra (normalized by [O III]λ5007) showing the key spectral features in the stacked spectra of the LyC leaking regions (blue) and nonleaking regions (red). The corresponding error spectra are shown in the dotted blue lines (leaker) and the dotted red lines (nonleaker).
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: The ionization diagram showing the location of the leaker (blue) and the nonleaker (red), using combined broad and narrow components. The gray squares represent SDSS data points and the green circles are z ∼ 2.3 galaxies from the MOSDEF survey (Sanders et al. 2016). The dotted line represents the AGN/star formation demarcation from Kauffmann et al. (2003).
Paper: The Connection Between Galactic Outflows and the Escape of Ionizing Photons
Authors: Ramesh Mainali, Jane R. Rigby, John Chisholm, Matthew Bayliss, Rongmon Bordoloi, Michael D. Gladders, T. Emil Rivera-Thorsen, Håkon Dahle, Keren Sharon, Michael Florian, Danielle A. Berg, Soniya Sharma, M. Riley Owens, Karin Kjellgren, Keunho J. Kim, Julia Wayne
Figure caption: HST WFC3/IR G141 grism spectrum of a LyC leaking region (knot 3) in the Sunburst Arc. The black line represents the grism spectrum, the dotted red line shows the noise level, and the blue line shows the best fit to the data.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Left: X-ray, optical, and radio light curves of GRB 160821B with the best-fit curve of the synchrotron afterglow model. The synchrotron light curves are shown at 1 keV (gray), the z band (purple), the F606W filter (dark red), the R band (salmon), the F110W filter (cyan), the F160W filter (light blue), the Ks  band (dark blue), the X-channel (olive), and the C-channel (emerald green). Data points are taken from Troja et al. (2019a). Right: broadband SEDs of the X-ray, optical, and radio afterglow observations with the best-fit synchrotron curves (lines) at 2 hr (red), 2 days (blue), and 4 days (green). The shaded areas correspond to blackbody spectra with decreasing temperatures from Troja et al. (2019a).
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Left: X-ray light curves with the optical upper limits of GRB 150101B with the best-fit curve of the synchrotron afterglow model. The synchrotron light curves are shown at 1 keV (gray), the R band (blue), the F606W filter (orange), and the F160W filter (green). Data points are taken from Fong et al. (2016) and Troja et al. (2018). Right: broadband SEDs of the X-ray, optical, and radio afterglow observations and upper limits with the best-fit synchrotron curves (lines) at 2 (red) and 9 (green) days. The red shaded region corresponds to the spectrum of AT 2017gfo, which is adapted by Troja et al. 2018.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Optical (u- and r-band) upper limits for GRB 050906, GRB 070810B, GRB 080121, and GRB 100216A with a set of synchrotron light curves evolving in a constant-density medium. The dashed and dotted lines are shown with n = 1 cm−3 and n = 10−2 cm−3, respectively. The parameter values used are E = 5 × 1050 erg, θ j = 3°, θ obs = 15°, Γ = 100, ε e = 0.3, p = 2.5, ζ  e  = 1.0, and ε B = 10−4. Upper limits are taken from Dichiara et al. (2020).
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: The X-ray, optical, and radio light curves of GRB 140903A with the best-fit curve of the synchrotron afterglow model. The synchrotron light curves are shown at 1 keV (blue), R band (gold), i band (brown), 9.8 GHz (dark green), and 6.1 GHz (light green). Data points are taken from Troja et al. 2016.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: The X-ray data points of SN 2020bvc with the best-fit curve obtained with the model presented in this paper for a stratification parameter of k = 1.5. The synchrotron light curve is shown at 1 keV. Data points are taken from Izzo et al. (2020).
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Diagram of bulk Lorentz factors and luminosities for the GRBs discussed in Fan et al. (2012) and Lü et al. (2012) and for sGRBs described in this work. The red dashed line corresponds to the best-fit ﹩{\rm{\Gamma }}=a{({\rm{L}}/{10}^{52}\,\mathrm{erg})}^{b}﹩ with a = (3.27 ± 0.39) × 102 and b = −(4.9 ± 0.20) × 10−2.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Same as Figure 4 but for SN 2020bvc.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Same as Figure 4 but for GRB 160821B.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Same as Figure 4 but for GRB 150101B.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Glitch size Δν, interglitch spin-down rate ﹩{\dot{\nu }}_{\mathrm{ig}}﹩, and time to next glitch T g for PSR J0537−6910 from NICER (large circles) and RXTE (small circles), with the latter from Antonopoulou et al. (2018), and for 16 other pulsars (crosses; errors not shown since they are smaller than the symbols in most cases) from Lower et al. (2021). Dotted lines are I sf/I = 0.001, 0.01, 0.1 [see Equation (3), where ﹩{\dot{\nu }}_{\mathrm{ig}}﹩ is ﹩\dot{\nu }﹩ between glitches and entrainment is neglected].
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: A direct comparison between the visual light curve of the 2005 classical nova eruption from AAVSO (left) and the OGLE I-band light curve of the 2019 outburst (right). The remarkable difference between the two light curves indicates that the two events are of a completely different nature.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Interglitch ﹩{\ddot{\nu }}_{\mathrm{ig}}﹩, glitch size ﹩{\rm{\Delta }}\dot{\nu }﹩, and time to next glitch T g for PSR J0537−6910 from NICER (large circles) and RXTE (small circles), with the latter from Antonopoulou et al. (2018), and for 16 other pulsars (crosses, i.e., all data shown with ﹩{\ddot{\nu }}_{\mathrm{ig}}\lt 3\times {10}^{-21}\,\mathrm{Hz}\,{{\rm{s}}}^{-2}﹩) from Lower et al. (2021). Dotted line is ﹩{\ddot{\nu }}_{\mathrm{ig}}=| {\rm{\Delta }}\dot{\nu }| /{T}_{{\rm{g}}}﹩ [see Equation (5)].
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Multi-band light curves of the 2019 outburst of V1047 Cen. The top panel shows optical and IR photometry from AAVSO (BVRI), OGLE (I), SMARTS (JHK), and NEOWISE (W1 and W2) photometry. The middle panel shows Swift UVOT UV data, and the bottom panel shows MeerKAT L-band radio flux at 1.28 GHz. Colors and symbols are coded as indicated in figure legends.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Extinction-corrected SED plot, showing the UV to radio SED of V1047 Cen on day 308. The error bars are 1σ uncertainties and they include contributions from the photometric and extinction uncertainties. We also present a zoom-in on the IR/optical/UV data.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: MeerKAT radio light curve measured at 1.28 GHz is plotted in the top-left panel, for comparison with three radio spectra measured on days 256, 294, and 700. Spectral indices are listed in each panel. The vertical dashed lines on the light-curve plot signify the epochs when spectra are measured.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Evolution of the extinction-corrected broadband colors (B − V)0, (V − R)0, and (R − I)0, throughout the outburst.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: TESS light curve of the 2019 outburst of V1047 Cen during sectors 11 (left) and 28 (right).
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Progression of the minifilament eruption in IRIS spectra (from bottom to top). Panels (a1)–(a3), (b1)–(b3), (c1)–(c3), and (d1)–(d3) show the spectra in the Mg II k line along the four slit positions of Figure 4(a) at three times. Slits 1, 2, and 3 cross the minifilament and the jet spire, and slit 4 crosses the JBP. The white dashed boxes are centered on the minifilament and JBP. In (d1)–(d3), the center of the JBP brightens under the erupting minifilament. The green arrows (in (a2) and (b2)) point to the shift of the minifilament toward shorter wavelength, whereas the white arrows (in (c1) and (d3)) point to the extension of the JBP toward longer wavelength.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Coronal jet observed in a coronal hole on 2020 April 8. (a) An AIA 211 Å image and (b) an IRIS 1400 Å SJI of the coronal hole during the jet. The white arrow points to the site of jet base brightening. The white box outlines the FOV in Figure 2. The two vertical dashed lines bound the area that is scanned by the IRIS slit.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Canceling magnetic flux at the magnetic neutral line under the minifilament. (a) The HMI LOS time–distance image along the red dashed line of Figure 2(k). Panels (b) and (c), respectively, display the decline of the jet-base absolute negative and positive magnetic flux with time before and through the eruption. The plotted negative and positive magnetic fluxes are those measured in the yellow box in Figure 2. The red dashed line marks the slow-rise start time of the minifilament. The blue line is the least-squares fit to the plotted negative or positive flux.