adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of a Dense Group of Hypercompact Radio Sources in the Central Parsec of the Galaxy
Authors: Jun-Hui Zhao, Mark R. Morris, W. M. Goss
Figure caption: Radial distribution of surface density of radio compact sources detected at the Galactic center. The red points are the surface-density data ﹩{{\rm{\Sigma }}}_{\mathrm{crs}}^{* }﹩ corrected for a higher equivalent sensitivity cutoff at 5.5 GHz by multiplying a correction factor η = 2.4 (see Equations (A13) and (A14)) to the original 33 GHz surface-density data Σcrs (light-gray points) derived from the 33 GHz observations of the HCRs (this paper). The black points mark the data of GCCRs observed at 5.5 GHz. In the annular zones around R = 3″, a bump in Σcrs is present. The orange line shows the best fitting to the power-law function with Γ = 1.6 ± 0.2 for the inner region, and the blue line indicates the least-squares fitting to the steeper power law with β = 2.0 ± 0.2 for the outer region. The break radius R  b  is ∼ 30″, or ∼1.2 pc. Three panels show the surface-density distributions for the three combinations of spectrum classes of HCRs: (a) including all the HCRs, (b) excluding the flat-spectrum HCRs, and (c) only including inverted HCRs.
Paper: H2 Cooling and Gravitational Collapse of Supersonically Induced Gas Objects
Authors: Yurina Nakazato, Gen Chiaki, Naoki Yoshida, Smadar Naoz, William Lake, Yeou S. Chiou
Figure caption: The projected distribution of gas and dark matter around gas cloud S1 from z = 31 to z = 25. The dense gas cloud S1 is formed at z = 25 and appears in the center of the right panel. The initial SV is imposed in the direction from left to right. The color map indicates the gas number density (see the color bar on the right), whereas the contours show the DM mass density distribution. The contour lines with white, pink, and red indicate 2, 20, and 200 times the critical density, respectively. The cross mark indicates the mass center of S1 and the black line indicates the S1 ellipsoid. We show the region with a side length of 40 comoving kpc.
Paper: H2 Cooling and Gravitational Collapse of Supersonically Induced Gas Objects
Authors: Yurina Nakazato, Gen Chiaki, Naoki Yoshida, Smadar Naoz, William Lake, Yeou S. Chiou
Figure caption: Large-scale distributions of gas and dark matter. The upper-left color map shows the DM column density in Run 0vH2. We plot the projected gas number density distributions in our simulations without SV (Run 0vH2, upper right) and with SV (Run 2vH2, bottom right). Run 2vH (bottom left) includes SV but not H2 cooling. We use the outputs at z = 25. The DM distribution is almost the same in all three runs. Each color map shows a region with a side length and a depth of 400 comoving kpc. In Run 2vH2, SIGO (S1) is located at the center of the figure, as indicated by an X mark.
Paper: H2 Cooling and Gravitational Collapse of Supersonically Induced Gas Objects
Authors: Yurina Nakazato, Gen Chiaki, Naoki Yoshida, Smadar Naoz, William Lake, Yeou S. Chiou
Figure caption: Top: the phase distribution of gas of S1 at z = 21.4. The white line shows the median at each density bin. The gray bands are the qth percentiles of the gas cells with q = 5, 10, 25, 50 (median), 75, 90, and 95. We plot the gas cells with n gas > 10−2.6 cm−3 around S1. Bottom: radial profiles of the ratio of the enclosed gas mass to the Jeans mass. M enc/M  J  ≧ 1 indicates that the SIGO S1 is Jeans unstable.
Paper: H2 Cooling and Gravitational Collapse of Supersonically Induced Gas Objects
Authors: Yurina Nakazato, Gen Chiaki, Naoki Yoshida, Smadar Naoz, William Lake, Yeou S. Chiou
Figure caption: The projected gas distribution around S1 at z = 25 and at z = 21.4, when S1 becomes Jeans unstable. The contour lines with white, pink, and red indicate the DM density of 2, 20, and 200 times the critical density. Both panels show the region around S1 with a side length of 1 physical kpc. The high-resolution simulation shown here is performed with the refinement of gas cells.
Paper: Common Envelope Jet Supernova r-process Yields Can Reproduce [Eu/Fe] Abundance Evolution in the Galaxy
Authors: Aldana Grichener, Chiaki Kobayashi, and Noam Soker
Figure caption: The [Eu/Fe] over [Fe/H] distribution in the Milky Way due to the contribution of common envelope jet supernovae that produce a europium mass of MEu = 2 × 10−5M⊙ and have delay times of td = 10 Myr (orange large dots), td = 20 Myr (yellow large dots), and td = 30 Myr (purple large dots). The black dots represent observational data taken from Cayrel et al. (2004), Honda et al. (2004), Hansen et al. (2012, 2014), Roederer et al. (2014), and Zhao et al. (2016).
Paper: Common Envelope Jet Supernova r-process Yields Can Reproduce [Eu/Fe] Abundance Evolution in the Galaxy
Authors: Aldana Grichener, Chiaki Kobayashi, and Noam Soker
Figure caption: Same as Figure 1, but for common envelope jet supernovae with a delay time of td = 20 Myr that produce europium masses of MEu = 1 × 10−5M⊙ (orange large dots), MEu = 2 × 10−5M⊙ (yellow large dots), and MEu = 3 × 10−5M⊙ (purple large dots).
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: Detrended TESS and ground-based transit light curves of TOI-1268b. In total we obtained 13 TESS transits in 2 minute cadence from Sectors 15, 21, 22, and 41, and 8 more full or partial transits from ground-based observatories. The Deep Sky West (DSW; simultaneously with TESS Transit 4) and Haleakala (simultaneously with TESS Transit 5) observations are jointly fitted with the TESS transits. The blue curves present the best-fit transit models.
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: Long-term photometric and spectroscopic observations of TOI-1268 using KELT, TESS, and TRES. Only a fraction of the KELT and TESS light curves are presented due to the limited space. The stellar rotation period is clearly detected in KELT and TESS photometry in the Lomb–Scargle periodogram. Neither stellar rotation period nor planetary orbital period is detected in TRES data. Applying a rotational kernel in Gaussian Process (GP) on KELT, TESS, and TRES data (see Section 3), we infer the stellar rotation period as 10.84 ± 0.07 days, consistent with the periodogram results. The blue curves are predicted GP models, and the light blue curves are drawn from posteriors.
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: Upper: the 5σ contrast curves of TOI-1268 from Palomar in the Brγ filter from adaptive optics (AO) imaging, and from Gemini North in the 832 nm and 562 nm bands from speckle imaging. Lower: the AO image (left) and reconstructed speckle image (right) of TOI-1268. No nearby companions are identified.
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: (a) Rotation period versus effective temperature of TOI-1268 (black star with red edge) and its neighboring stars in comparison with clusters groups with well-determined ages. The clusters we used are 120 Myr Pleiades (blue circles, Rebull et al. 2016), 250 Myr MELANGE-1 (blue squares, Tofflemire et al. 2021), 250 Myr Group X (green diamonds, E. Newton et al. 2022, in preparation), 670 Myr Praesepe and 730 Myr Hyades (orange and red circles, Douglas et al. 2016, 2019), 1 Gyr NGC 6811 (cyan circles, Curtis et al. 2019), and 2.5 Gyr NGC 6819 (purple triangles, Meibom et al. 2015). For stars we identified with the Comove package, the ones with rotation period and effective temperature consistent with TOI-1268 are plotted with dark gray crosses, while the ones that deviate from it are plotted with light gray crosses. (b) Lithium equivalent width (EW) vs. effective temperature of TOI-1268 (red star) and its neighboring stars in comparison with clusters groups with well-determined ages. The clusters we used are 120 Myr Pleiades (blue circles), 250 Myr Group X (green circles, E. Newton et al. 2022, in preparation), and 670 Myr Praesepe (orange circles).
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: (a) and (b) In-transit radial-velocity measurements of the TOI-1268 system using the NEID spectra. The blue dots and black bars are NEID RVs and their corresponding uncertainties. Using the RM effect, the projected stellar obliquity is constrained. (c) The Doppler tomography signal of the TOI-1268 system during TOI-1268b’s transit. The left, middle, and right panels are data extracted from the NEID spectra, best-fit model, and the residual of the data after subtracting the best-fit model. The color scale presents the flux variation of the velocity channel. We expect to observe a decrease in flux in the velocity channel of the star blocked by the planet.
Paper: NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
Authors: Jiayin Dong, Chelsea X. Huang, George Zhou, Rebekah I. Dawson, Gumundur K. Stefánsson, Chad F. Bender, Cullen H. Blake, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Daniel J. Stevens, Ryan C. Terrien, Andrew Vanderburg, Adam L. Kraus, Stephanie Douglas, Elisabeth Newton, Rayna Rampalli, Daniel M. Krolikowski, Karen A. Collins, Joseph E. Rodriguez, Dax L. Feliz, Gregor Srdoc, Carl Ziegler, Khalid Barkaoui, Francisco J. Pozuelos, Emmanuel Jehin, C. Michaël, Zouhair Benkhaldoun, Pablo Lewin, Raquel Forés-Toribio, Jose A. Muñoz, Kim K. McLeod, Fiona Powers Özyurt, Ferran Grau Horta, Felipe Murgas, David W. Latham, Samuel N. Quinn, Allyson Bieryla, Steve B. Howell, Crystal L. Gnilka, David R. Ciardi, Michael B. Lund, Courtney D. Dressing, Steven Giacalone, Arjun B. Savel, Ivan A. Strakhov, Alexander A. Belinski, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Guillermo Torres, and Martin Paegert
Figure caption: Projected stellar obliquity vs. estimated stellar age for all hot/warm Jupiters. Planets are colored by a/R⋆ and labeled in triangles or circles given their host star effective temperatures (i.e., triangles for host stars above the Kraft break Teff > 6250K and circles for stars below the Kraft break). Gray lines show 1σ uncertainties. For TOI-1268, we plot its estimated age between the 120 Myr Pleiades and 670 Myr Praesepe clusters and its stellar obliquity using representative values inferred from SERVAL RVs labeled in blue error bars. The 3σ credible interval of obliquity posteriors derived from the RV and DT signals are shown in black.
Paper: Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for Hα and White-light Emissions
Authors: Kosuke Namekata, Hiroyuki Maehara, Satoshi Honda, Yuta Notsu, Soshi Okamoto, Jun Takahashi, Masaki Takayama, Tomohito Ohshima, Tomoki Saito, Noriyuki Katoh, Miyako Tozuka, Katsuhiro L. Murata, Futa Ogawa, Masafumi Niwano, Ryo Adachi, Motoki Oeda, Kazuki Shiraishi, Keisuke Isogai, Daisaku Nogami, and Kazunari Shibata
Figure caption: Superflares on EK Dra detected by TESS (Sector 14–16 and Sector 21–23). (A) The TESS light curve of Sector 14–16 (2019 July 18–2019 October 7) normalized by the average flux. (B) The detrended light curve of the panel (A). The times of the automatically detected flares are indicated by red lines. (C) The TESS light curve during Sector 21–23 (2020 January 21–2020 April 15) normalized by the average flux. (D) The detrended light curve of the panel (C). The periods of the monitoring observations by the Seimei telescope/KOOLS-IFU are marked in blue. Flares detected by ground-based telescopes on 14 March 2020 (this Letter) and 5 April 2020 (Namekata et al. 2021) are also shown in green and cyan, respectively. Note that the detrended light curve is automatically obtained by a low-pass filter without removing the flares, and background subtraction is different from Figure 2(A) (see Section 2.1 for the analysis). (E) The flare frequency on EK Dra detected by TESS. The flare frequency of EK Dra in X-rays, as determined by Audard et al. (1999), is shown as a black line for reference. The red solid line corresponds to the fitted one (N(>E) ∝ E−0.72±0.01) for 2 × 1033 to 2 × 1034 erg. (F) The relationship between flare energy and duration as determined by TESS. The gray cross points are the relationship between energy and duration obtained by Kepler (Maehara et al. 2015). The theoretical scaling relation with constant flare loop length (1010, 3 × 1010, and 1011 cm) is shown by the dashed line (Namekata et al. 2017).
Paper: Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for Hα and White-light Emissions
Authors: Kosuke Namekata, Hiroyuki Maehara, Satoshi Honda, Yuta Notsu, Soshi Okamoto, Jun Takahashi, Masaki Takayama, Tomohito Ohshima, Tomoki Saito, Noriyuki Katoh, Miyako Tozuka, Katsuhiro L. Murata, Futa Ogawa, Masafumi Niwano, Ryo Adachi, Motoki Oeda, Kazuki Shiraishi, Keisuke Isogai, Daisaku Nogami, and Kazunari Shibata
Figure caption: White light and Hα light curves of the superflare and rotation variations on EK Dra observed on 2020 March 14. (A) The black line is the observed TESS light curve at the rotation phase when the superflare occurred. The orange dashed line is one fitted with the FFT and low-pass filter. The upper right in panel (A) is an enlarged light curve where the flare occurred. (B) The detrended TESS light curve (i.e., the black minus orange line in panel (A)). (C) The rotational modulation of the Hα EW folded by the rotational period (Prot = 2.62 days and t0 = BJD-2458923). The different colors plot different rotational phases, and the red data are the rotation phase when the superflare occurred. The dashed line is a line fitted with a simple sine function for these rotation variations. The EW is the integrated Hα absorption between 6552.8 and 6572.8 Å, normalized by the continuum level of 6517.8–6537.8 Å and 6587.8–6607.8 Å. (D) The Hα light curve of the superflare (red) and its background level (black). The background model derived from the data on March 14 is consistent with the March 11 data. (E) The light curves of the superflare observed in Hα (red) and TESS white light (black). The lack of Hα data at approximately BJD-2458923 + 4 hr is due to the temporary cloud in the sky. The dashed line is the assumed background level for each.
Paper: Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for Hα and White-light Emissions
Authors: Kosuke Namekata, Hiroyuki Maehara, Satoshi Honda, Yuta Notsu, Soshi Okamoto, Jun Takahashi, Masaki Takayama, Tomohito Ohshima, Tomoki Saito, Noriyuki Katoh, Miyako Tozuka, Katsuhiro L. Murata, Futa Ogawa, Masafumi Niwano, Ryo Adachi, Motoki Oeda, Kazuki Shiraishi, Keisuke Isogai, Daisaku Nogami, and Kazunari Shibata
Figure caption: The temporal evolution of Hα line profiles of the superflare on EK Dra. (A) Temporal variation of the pre-flare-subtracted Hα spectra in the time–wavelength plane. The color bar shows the emission intensity normalized by the continuum level (6517.8–6537.8 Å and 6587.8–6607.8 Å). (B) The Hα spectra of the superflare on 2020 March 14 observed with the Seimei Telescope/KOOLS-IFU. Each colored spectrum indicates the 20 minute averaged spectrum during the superflare with the central time indicated in the panel and the background black dashed line is the pre-flare template spectrum. The pre-flare template spectrum was created by averaging the first 35 pieces of data for the night (−0.35 hr to 0.15 hr in panel (A)). The spectra are normalized by the continuum level and the constant values are added for visibility. The dotted vertical line indicates the line center. (C) The pre-flare subtracted spectra of those in the panel (B). The basal level of each spectrum is plotted with the horizontal dashed line.
Paper: Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for Hα and White-light Emissions
Authors: Kosuke Namekata, Hiroyuki Maehara, Satoshi Honda, Yuta Notsu, Soshi Okamoto, Jun Takahashi, Masaki Takayama, Tomohito Ohshima, Tomoki Saito, Noriyuki Katoh, Miyako Tozuka, Katsuhiro L. Murata, Futa Ogawa, Masafumi Niwano, Ryo Adachi, Motoki Oeda, Kazuki Shiraishi, Keisuke Isogai, Daisaku Nogami, and Kazunari Shibata
Figure caption: The Hα line profiles of the superflare on EK Dra. (A, B) The pre-flare-subtracted Hα spectra at t = 0.9 and 2.45 minutes, respectively. The blue lines result from the one component fitting with Voigt function. The red vertical lines correspond to the fitted line center. The line centers are 16.7 ± 4.1 km s−1 and 26.6 ± 4.8 km s−1, as indicated in each panel. The FWHM of the lines are 5.4 and 5.0 Å, as also indicated in the panels. (C, D) The black data are the same as the panels (A) and (B), respectively. The colored line in the panels (C) and (D) are the results of two-component fitting with a Voigt function (orange line for the central component) and Gaussian function (green line for the redshift component). We first fitted the blue-wing profile with a Voigt function and fitted the residual of the red wing with the Gauss function. The red lines are the sum of the green and orange lines. The central velocity of the Gaussian (green lines) components of panels (C) and (D) are 99 ± 13 km s−1 and 108 ± 7 km s−1, respectively. The other properties of the red-wing enhancement are summarized in Table 1.