adsabs/AstroCLIMB huggingface dataset:
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: IRIS SJI images from the 2022 March 30 X-class flare, showing a sequence of 2796 Å observations. They show the initial brightening in the region of our source of interest, and then the rebrightening of this source a few minutes later. A rectangular box outlines the source of interest. The second brightening is associated with the appearance of extremely broad red wings of several spectral lines. For one frame (at 17:35:19 UT), a small bright feature appears near x = 512″, y = 299″. By the next exposure, it is no longer present. This feature could be a small extension of the southern ribbon, reappearing in a region that was previously brightened. The darker vertical line in each image is IRIS’ spectrograph slit. The distorted feature in the bottom of the image, extending from x = 510″–514″ is the result of dust on the detector, which appears bright here since the image is shown on a logarithmic scale. Appendix A shows a similar figure for the 1330 Å filter.
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Multi-Gaussian fit of UV spectra at 17:35:19 UT on SOI (Y = 51 pixel). Three Gaussian components are involved, and the combinations of all components are the modeled results in red solid curves. The dotted–dashed line in yellow is the red-most Gaussian fit, representing the downward Doppler velocities. The relative timing of these spectra are indicated by thick horizontal lines on Figure 4. The vertical line in each panel shows the rest line center positions of C II, Si IV, and Mg II, at 1334.53 Å, 1402.77 Å, and 2796.33 Å, respectively.
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Evolution of derived redshift velocities, using a multi-Gaussian fit in panels (a)–(d) and the spectral-moments method in panels (e)–(h), on SOI (Y = 51 pixel).
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: (a) SDO/AIA 211 Å image taken at 17:35:25 UT, showing two major flare ribbons and flaring loops. (b) SDO/AIA 1600 Å image taken at 17:35:26 UT. (c) IRIS SJI 2796 Å image in the same field of view as the AIA image, taken at 17:35:08 UT. The dark line indicates the slit position, and the small red box SOI indicates the region of interest. (d) Light curves of GOES soft X-ray (SXR, in black), derivative of SXR (red), UV-2796 in SOI (green).
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Mg II line profiles in 2014 March 29 flare (blue) at 17:46:13 UT on pixel (436) and 2022 March 30 flare (red) at 17:35:19 UT on pixel (51). The intensity of the line profile of 2014 March 29 flare is reduced by a factor of 10.
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Same as Figure 4, but for the O I 1355.598 Å and C I 1355.884 Å lines (top panel), and O IV 1401.163 Å (bottom panel).
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Histogram of Mg II redshifts of pixels on flare ribbon (orange) and SOI region (blue).
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: The left, middle, and right panels show PV diagrams along the major axis for the 13CO, C18O, and SO molecules, respectively. A 5-pixel average (∼0.″5) PV profile was obtained in all the figures. The white contours mark the emission at 5σ, 15σ, and 25σ to match the contours shown in their channel maps (Figures B2, B3, and B4 in Appendix B). The dashed white contours in the CO molecules show the negative emission at −3σ, −6σ, and −9σ caused by continuum oversubtraction. The ridge and edge methods to trace the disk emission are marked by filled circles and triangles. The results from SLAM indicate that the inner portions of the velocity profiles can be reproduced by a central protostellar mass of ∼0.5 M ⊙.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Left: a streamer model overlaid on the moment 0 map of the C18O emission. The model was used to reproduce three features: the conspicuous northern streamer that divides into a northeast and a northwest branch, and the short eastern arm. The dashed oval corresponds to the size of the quasi-Keplerian radius of 265 au as calculated from SLAM. Right: the projected distance along the streamer vs. velocity is shown for the northwest, northeast, and east streamers, as labeled. The white dashed lines show the spatial and velocity trails of the models that delineate the observed PV diagrams. The horizontal cyan lines mark the distance at which the infalling streamers transition to a mostly Keplerian velocity. The thin red lines marks the systemic velocity at V sys = 2.8 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Left: a streamer model overlaid on the moment 0 map of the SO emission. We attempted to reproduce the three SO spirals. The dashed oval corresponds to the size of the Keplerian radius of 110 au as calculated from SLAM. Right: the projected distance along the streamer versus velocity is shown for spirals, as labeled. The white dashed lines show the spatial and velocity trails of the models that delineate the observed PV diagrams. The horizontal cyan lines mark the distance at which the infalling streamers should be affected by Keplerian rotation. The thin red lines marks the systemic velocity at V sys = 2.8 km s−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Channel map of the SO emission in Oph IRS 63. The lowest contour emission corresponds to 5σ or 22 mJy beam−1, with increments of 10σ at a time. The FOV of the map is 8″ × 8″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Schematic view of the system’s large-scale emission. The gray rotating structure represents the envelope observed in 13CO and C18O at radial offset ≥2″. The red arrows mark the portion of the envelope receding, while the blue ones mark emission toward us. The wide outflows and the narrow blueshifted outflow are also depicted. The blueshifted outflow partially blocks the view toward the lower right part of the envelope owing to geometrical effects.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Channel map of the 12CO emission in Oph IRS 63. The lowest contour emission corresponds to 6σ or 12 mJy beam−1, with increments of 12σ at a time. The FOV of the map is 26″ × 26″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Channel map of the 13CO emission in Oph IRS 63. The lowest contour emission corresponds to 5σ or 22.5 mJy beam−1, with increments of 10σ at a time. The FOV of the map is 24″ × 24″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Channel map of the C18O emission in Oph IRS 63. The lowest contour emission corresponds to 5σ or 15 mJy beam−1, with increments of 10σ at a time. The FOV of the map is 24″ × 24″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: iSHELL K-band spectrum of Oph IRS 63 centered around the Brγ line at 2.166 μm. The green shaded region depicts the region integrated to obtain (proto)stellar mass accretion rate. This spectrum shows the flux before extinction correction.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Evolution of the power-law index α, L, and the Alfvén time t  A  during the flux emergence and relaxation phase with a rate of 4.52 G hr–1. The black vertical line indicates the time when the emergence has finished. The green horizontal line represents the critical α triggering the Sweet–Parker reconnection (﹩\tfrac{1}{2}﹩), and the red horizontal line denotes the critical α for the establishment of ideal tearing (﹩\tfrac{1}{3}﹩). The third panel shows the evolution of t  A  = L/v  A . One can see that it remains close to 3 minutes during the whole emergence phase, while the CS length doubles in size and follows linearly the evolution of the Alfvén speed increase in the bipole.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Figure depicting the periodicity of oscillation of radial velocity and EUV 193 Å for (a) different emergence rates (G hr–1) but a fixed diffusivity of 1012 cm2 s−1 and (b) different magnetic diffusivity values for the same emergence rate 4.52 G hr–1.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Wavelet analysis of the radial velocity for the setup of a flux emergence of 4.52 G hr–1 and η = 1012 cm2 s−1. (a) Radial velocity evolution over time at 1.5 R ⊙, the detrended radial velocity after subtracting it from the original gray (color). (b) The wavelet power spectrum of the detrended signal is displayed as well as (c) the global wavelet power spectrum.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: A 2D map of density fluctuations (δ ρ) relative to the local density ρ. δ ρ is computed by subtracting two consecutive frames separated by a 16 minute time lapse.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: The maximum values of the radial velocity simulated in the plume above the CS at a distance of approximately 1.5 R ⊙ for the different setups of flux emergence. Magnetic diffusivity was fixed in all simulations at η = 1012 cm2 s−1.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: In the upper panel, we plot the evolution of CS length (L) for all setups with η = 1012 cm2 s−1 and the second panel shows the linear fit with the corresponding slope “s.”
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Synthetic EUV emission intensity maps produced from the simulation results for two wavelengths observed by the SDO. These emission intensity maps were produced from the simulation setup with a flux emergence rate of 4.52 G hr–1.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Synthetic emission intensities of the 193 Å EUV line for the four emergence rates simulated for a fixed η = 1012 cm2 s−1.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Density and velocity perturbations as a function of time for an emergence rate of 9 G hr–1 at 1.15 R ⊙ in the jet’s stalk.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Spectral fitting examples of type 1 AGN ([7]J074704). Left: Hβ & [O III] region. The best-fit model (red) is compared with the observed spectrum (black). NLR core (green), NLR wing (blue), BLR (magenta), and the continuum emission (power-law + Fe II , cyan) are fitted simultaneously. Right: Hα, [N II] & [S II] region. The power-law continuum is subtracted before the emission line fitting. The best-fit model (red) is compared with the continuum-subtracted residual spectrum (black). NLR core (green) and BLR (magenta) are included in the model for this target.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: [O III] VVD diagram of the GMOS sample, which is composed of type 1 (blue) and type 2 AGNs (red stars) in this study and type 2 AGNs (red circles) in our previous studies (Karouzos et al. 2016a, 2016b; Kang & Woo 2018; Luo et al. 2019). Blue and red dots represent the parent SDSS samples of type 1 AGNs (Rakshit & Woo 2018) and type 2 AGNs (Woo et al. 2016), respectively.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Spectral fitting examples of type 2 AGN ([13]J083132). The stellar continuum is subtracted before the emission line fitting. The best-fit models (red) are compared with the continuum-subtracted residual spectra (black) for Hβ & [O III] region (left panel) and Hα, [N II] & [S II] region (right panel). NLR core (green) and wing (blue) components are included in the model.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity maps of [O III] (top) and Hα (bottom) emission lines. The blue color indicates a blueshift, i.e., approaching kinematics, while the red color indicates a redshift, i.e., receding kinematics. Note that Hα velocity map of [15]J211307 is replaced with [N II] due to the saturated columns in the CCD.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: SDSS Optical gri-composite images of the GMOS-IFU sample in this work. Each panel shows a 20″ × 20″ scale, while the FOV of GMOS-IFU (3.″5×5″) is denoted with a green box.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Flux maps of [O III] (top) and Hα (bottom) emission lines. The gray area represents the spaxels where the emission line is not detected (i.e., A/N < 3). Note that Hα flux map of [15]J211307 is not shown here due to the saturated columns in the CCD.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity dispersion maps (i.e., the second moment maps) of [O III] (top) and Hα (bottom) emission lines. Note that Hα velocity dispersion map of [15]J211307 is replaced with [N II] due to the saturated columns in the CCD.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: High-EP lines in the HIRES spectra of V960 Mon, smoothed with a σ = 5 pixel Gaussian for clarity. Epochs are shown in different colors, where redder indicates later epochs when the target is dimmer and, according to our disk model, cooler. The black vertical lines mark ±60 km s−1, the estimated v max at outburst, as a reference for the line widths. The C I λ9095 line is significantly contaminated by telluric absorption, but its similar evolution to the other lines is still apparent.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The Na D λ5889 line (top row) and Ca II IRT lines (lower three rows), shown in the data (left column) and residuals (right column). The Ca II IRT lines show a weakening fast blueshifted component and a ±60 km s−1 emission component similar to those seen in the H lines. Note that the +100 km s−1 absorption is due to HP line blending with the IRT. This is well matched by our disk model and mostly removed in the residuals column. The Na D lines are saturated from −10 to 0 km s−1, which matches the narrow absorption seen in the latest epoch, indicating there may be a constant slow wind covering almost the entire visible emission region of the disk.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The Hβ and Hα lines in each of the HIRES epochs as seen in the original data (left) and as residuals after removing the disk contribution (right). Both lines initially show a high-velocity blueshifted absorption component that weakens rapidly over time and becomes an emission feature in Hα. The profiles also contain a slow component that moves redward. The emission components of the Hα profile are both peaked at ±60 km s−1 and strengthen consistently relative to the continuum. The absorption in the upper left panel at +185 km s−1 is the Cr II 4864 Å line. Notice it is well removed by the model and is much weaker in the upper right residual panel.