adsabs/AstroCLIMB huggingface dataset:
Paper: Transition Probabilities of Near-infrared Ce III Lines from Stellar Spectra: Applications to Kilonovae
Authors: Nanae Domoto, Jae-Joon Lee, Masaomi Tanaka, Ho-Gyu Lee, Wako Aoki, Miho N. Ishigaki, Shinya Wanajo, Daiji Kato, Kenta Hotokezaka
Figure caption: Enlarged view of the synthetic spectrum in the NIR region at t = 2.5 days. The blue curve shows the synthetic spectrum using the derived gf-values, and green curve shows that of Domoto et al. (2022). The orange and red curves show the synthetic spectra when using the lower and upper gf-values, which consider the sum of the uncertainties negatively and positively, respectively (see the text). The curves in light colors show the original results, while those in dark colors show smoothed spectra for visualization.
Paper: First Results for Solar Soft X-Ray Irradiance Measurements from the Third-generation Miniature X-Ray Solar Spectrometer
Authors: Thomas N. Woods, Bennet Schwab, Robert Sewell, Anant Kumar Telikicherla Kandala, James Paul Mason, Amir Caspi, Thomas Eden, Amal Chandran, Phillip C. Chamberlin, Andrew R. Jones, Richard Kohnert, Christopher S. Moore, Stanley C. Solomon, Harry Warren
Figure caption: Solar activity over the INSPIRESat-1 mission is shown for the GOES-16 XRS-B 1 minute averaged irradiance. The INSPIRESat-1 launch was on 2022 February 14. The GOES flare classes are indicated on the right axis. The times for the DAXSS solar observations are shown in green. The downlinked (DLINK) science packets as indicated in red are currently limited by the INSPIRESat-1 UHF communication system, but are anticipated to be increased significantly once its S-band ground station is commissioned.
Paper: Transition Probabilities of Near-infrared Ce III Lines from Stellar Spectra: Applications to Kilonovae
Authors: Nanae Domoto, Jae-Joon Lee, Masaomi Tanaka, Ho-Gyu Lee, Wako Aoki, Miho N. Ishigaki, Shinya Wanajo, Daiji Kato, Kenta Hotokezaka
Figure caption: Comparison between the synthetic spectra (blue) and the observed spectra of AT2017gfo taken with the VLT (gray; Pian et al. 2017; Smartt et al. 2017) at t = 1.5, 2.5, and 3.5 days after the merger (dark to light colors). The spectrum taken with the HST at t = 4.5 days after the merger (Tanvir et al. 2017) is also shown as a black line. The green curves are the synthetic spectra of Domoto et al. (2022; see their Figure 8). Spectra are vertically shifted for visualization. Gray shaded areas show the regions of strong atmospheric absorption.
Paper: First Results for Solar Soft X-Ray Irradiance Measurements from the Third-generation Miniature X-Ray Solar Spectrometer
Authors: Thomas N. Woods, Bennet Schwab, Robert Sewell, Anant Kumar Telikicherla Kandala, James Paul Mason, Amir Caspi, Thomas Eden, Amal Chandran, Phillip C. Chamberlin, Andrew R. Jones, Richard Kohnert, Christopher S. Moore, Stanley C. Solomon, Harry Warren
Figure caption: As compared to MinXSS-1, the DAXSS sensor has significant improvements in effective area (left panels) and energy resolution (right panels).
Paper: Transition Probabilities of Near-infrared Ce III Lines from Stellar Spectra: Applications to Kilonovae
Authors: Nanae Domoto, Jae-Joon Lee, Masaomi Tanaka, Ho-Gyu Lee, Wako Aoki, Miho N. Ishigaki, Shinya Wanajo, Daiji Kato, Kenta Hotokezaka
Figure caption: The observed spectra around the Ce III lines of the Ap stars. Absorption lines are labeled as in Figure 1.
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: Exposure time (ks) required for a 5σ detection of CX X-ray emission (Equation (B12)), as a function of the outgassing rate Q gas and perihelion distance r peri. The geocentric distance is fixed at Δ e  = 1 au. The background rate and effective area correspond to those of EPIC pn on XMM-Newton. For reference, the markers are plotted at locations representative of real minor bodies: light blue (“H”) corresponds to Q gas = 1.5 × 1029 s−1 observed at 1.0 au—similar to C/1996 B2 (Hyakutake); tan (“B”) corresponds to Q gas = 1027 s−1 observed at 2.0 au—similar to 2I/Borisov; and coral (“O”) corresponds to Q gas = 2.8 × 1028 s−1 observed at 0.25 au and Q gas = 1.8 × 1027 s−1 observed at 1.0 au—estimates corresponding to 1I/‘Oumuamua under a CO composition. The solar elongation angles of Chandra (﹩{\psi }_{\odot }^{{\min }}={46.4}^{^\circ }﹩) and XMM-Newton (﹩{\psi }_{\odot }^{min}={70}^{^\circ }﹩) impose lower bounds (﹩\sin {\psi }_{\odot }^{\min }﹩) on observable r  p , and their respective restricted zones are hatched in the figure. The lower bound is attained only in the ideal orbital case and observable heliocentric distances are typically significantly larger due to spacecraft limitations.
Paper: Redshift Evolution of Electron Density in the Interstellar Medium at z ∼ 0–9 Uncovered with JWST/NIRSpec Spectra and Line-spread Function Determinations
Authors: Yuki Isobe, Masami Ouchi, Kimihiko Nakajima, Yuichi Harikane, Yoshiaki Ono, Yi Xu, Yechi Zhang, Hiroya Umeda
Figure caption: Electron density n e as a function of M * (left), SFR (center), and sSFR (right). The large red circles and the large red double circles denote the median and 16th–84th percentiles of the properties of the JWST galaxies at z ∼ 4–6 and z ∼ 7–9, respectively. The small red circles and the small red double circles represent the properties of each JWST galaxy at z ∼ 4–6 and z ∼ 7–9, respectively. The other symbols are the same as those in Figure 3. The blue and green shaded regions correspond to the 16th–84th percentile ranges of the n e values of the galaxies at z ∼ 0–1 (Berg et al. 2012; Swinbank et al. 2019; Davies et al. 2021) and z ∼ 1–3 (Steidel et al. 2014; Sanders et al. 2016a; Kaasinen et al. 2017; Kashino et al. 2017; Davies et al. 2021), respectively. On average, the JWST galaxies have higher n e than lower-z galaxies at a given M *, SFR, and sSFR.
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: Schematic of SW CX with the outgassed neutrals in the coma of an ISO. Panel 1: an instantaneous view of the inner solar system and the trajectory of an ISO, currently at perihelion (r peri). Panel 2: the flux of solar radiation (F ⊙) heats the volatiles on the ISO’s surface, which causes the sublimation and outgassing of neutral volatiles at a rate Q gas. Panel 3: SW ions (with number density n SW) interact with the outgassed coma through CX. Electrons are transferred from the neutral coma to the bare or H-like SW ions and the subsequent cascade emits X-rays. The coma’s interaction cross section (﹩{ \mathcal A }﹩) scales with ﹩{Q}_{\mathrm{gas}}^{2}﹩. As a result, the X-ray luminosity follows ﹩{L}_{{\rm{X}}}\propto {r}_{\mathrm{peri}}^{-6}﹩ (Equation (5); Section 2.2).
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: Trajectory and X-ray observability of 1I/‘Oumuamua, prior to its discovery. The plotted lines connect the instantaneous positions of Earth and 1I/‘Oumuamua. The blue lines denote a solar elongation angle meeting X-ray observing requirements, ﹩{\psi }_{\odot }\geqslant {\psi }_{\odot }^{\min }﹩, where ﹩{\psi }_{\odot }^{\min }=70^\circ ﹩ for XMM-Newton. The smallest heliocentric distance allowed by this constraint is denoted R* = 0.943 au. At this time, the distance between Earth and 1I/‘Oumuamua was ﹩{{\rm{\Delta }}}_{e}^{* }=0.276\,\mathrm{au}﹩.
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: Cumulative distribution functions of X-ray flux (F X) for ISOs detected by the Rubin Observatory. Equivalently, the fractions of ISOs detected by the Rubin Observatory that will exhibit a given X-ray flux or less. Four distributions are depicted, each corresponding to an ISO population comprised of a different pure volatile: H2O (blue), CO (red), N2 (green), and H2 (orange). On the top x-axis, F X is converted into an exposure duration (τ 5σ ) that would yield a 5σ detection with the XMM-Newton EPIC pn. The vertical blue line delineates F X ≃ 2.7 × 10−15 erg s−1 cm−2—a signal that would be detected at 5σ confidence with a 10 ks exposure. For example, about 10% of CO-dominated ISOs detected by the Rubin Observatory will exhibit this X-ray flux or greater.
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: Time evolution of the production rates for 2I/Borisov near perihelion (for CO, H2O, and OH). Figure adapted from Seligman et al. (2022). The references for data are provided in their Table 2. The measurements demonstrate that the CO production was substantially greater than the H2O production after perihelion—the only time when both species were observed contemporaneously. Our production rate model (Equation (B8)) is plotted as dashed lines, holding 2I/Borisov’s radius as a constant a = 0.3 km and adopting an appropriate ﹩{ \mathcal H }﹩ for H2O and CO. We obtained 2I/Borisov’s heliocentric distance with a rebound (Rein & Liu 2012) simulation using the Mercurius integrator (Rein et al. 2019). For reference, the trajectory of 2I/Borisov through the solar system is shown in the right panel, with perihelion marked. The solid blue portion corresponds to the time span plotted in the left panel.
Paper: X-Rays Trace the Volatile Content of Interstellar Objects
Authors: Samuel H. C. Cabot, Q. Daniel Wang, Darryl Z. Seligman
Figure caption: The relationship between the outgassing rate Q gas and radius b within which a coma is optically thick to CX. Since b lacks a closed form (Equation (B6)), it is solved for numerically. The function is plotted for several assumptions of the ionization scale λ. In all cases, v = 1 km s−1. Our main analysis assumes λ = 5 × 1010 cm (the red line). As λ increases, the function approaches a linear relationship between Q gas and b (the black dashed line).
Paper: Redshift Evolution of Electron Density in the Interstellar Medium at z ∼ 0–9 Uncovered with JWST/NIRSpec Spectra and Line-spread Function Determinations
Authors: Yuki Isobe, Masami Ouchi, Kimihiko Nakajima, Yuichi Harikane, Yoshiaki Ono, Yi Xu, Yechi Zhang, Hiroya Umeda
Figure caption: Electron density n e as a function of redshift. All of the measurements in this figure are based on low-ionization lines (i.e., [O II] or [S II]). The symbols are the same as those in Figure 4. The dotted and dashed curves represent n e following the ∝(1 + z) and ∝(1 + z)2 relations, respectively, which are determined by the galaxies at z ∼ 0–3. The JWST galaxies lie on the gap between the two functions (i.e., n e ∝ (1 + z) and (1 + z)2) filled with gray shading.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: Top: the so-called “Δm–Δt” diagram of the ﹩\mathrm{log}\dot{M}﹩ variabilty. Each black point on the background represents a pair of ﹩\dot{M}﹩ measurements, with x values being the absolute difference in time (∣Δt∣), and y values being ﹩| {\rm{\Delta }}\mathrm{log}\dot{M}| ﹩. Individual pairs are bins in the order of ∣Δt∣ by every 500 pairs (orange points) or by every ∣Δt∣ = 0.033 (green points). The purple dashed line denotes the two-part function that fits the binned points best, with a break at ∼1.6 days from a power-law increase to a flat line (see Equation (4) and Table 9 for details). Bottom: the periodogram of the ﹩\mathrm{log}\dot{M}﹩ variability. The horizontal dashed and dotted lines represent the 5% and 1% false-alarm rates, respectively.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: Correlations between accretion luminosity and line luminosities (red circles from ESPaDOnS, black circles from other instruments), with a best-fit (solid pink line) and a comparison to the best-fit correlation (dashed blue line) for the relationships from Alcalá et al. (2017). For Hα 10% width, the comparison is to the correlation calculated by Natta et al. (2004), adjusted to accretion luminosity given the parameters for TW Hya. Some of the lines are poorly correlated with the accretion luminosity.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: Histograms of accretion rates, plotted as a distribution in linear (left) and logarithmic (right) values, with corresponding veiling on the top axis. The average ﹩\mathrm{log}\dot{{M}_{\mathrm{acc}}}﹩ is 10−8.65 M ⊙ yr−1 with a standard deviation of 0.22 dex. The differences in veiling are much larger than the precision and cross-instrument uncertainties of ∼0.02.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: Hα, Hβ, and two He I lines from an epoch with strong accretion (solid black line) and an epoch with weak accretion (red dashed line). The spectra shown here have had the photosphere subtracted and are then normalized to the relevant photospheric continuum to place the lines on the same flux scale. The He lines are brighter but the H lines are fainter during the epoch with stronger accretion, illustrating by example that accretion is more tightly correlated with He emission than with H emission. The H lines are formed in an optically thick medium and have emission that may be absorbed by the wind or accretion flow.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: Accretion rate of TW Hya (red rectangle), compared with accretion rates from Lupus and Cha I star-forming regions (black circles, Alcalá et al. 2017; Manara et al. 2017). The size of the thick rectangle for TW Hya shows the 1σ scatter of the accretion rates while the thin line shows the full range of accretion rates. The average accretion rate of TW Hya is only ∼0.1 dex fainter than and consistent with expectations, given the uncertainties, based on a linear fit to the relationship between ﹩\mathrm{log}{M}_{\mathrm{acc}}﹩ and ﹩\mathrm{log}{M}_{* }﹩.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: The Hα profile shows strong Lorentzian wings with emission that extends to ∼2000 km s−1 on both sides of the line profile. The spectrum shown here (black), from an epoch with strong accretion, is normalized by the photospheric continuum level. The photospheric template TWA 25 (blue spectrum) is scaled to the appropriate level based on the veiling and is then subtracted from the full spectrum to calculate the accretion spectrum (red).
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: He I absorption, seen here to ∼300–400 km s−1 in three lines on 2016 February 27, an epoch with strong accretion. The He II λ4686 line (bottom, pink) has emission that extends out to 450 km s−1.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: The full veiling lightcurve (top), with specific segments highlighted in the bottom six panels, with average veiling (horizontal line) and standard deviation (shaded yellow region). In the six panels, the date range in the x-axis differs in each plot.
Paper: Twenty-five Years of Accretion onto the Classical T Tauri Star TW Hya
Authors: Gregory J. Herczeg, 雷歌 沈, Yuguang Chen, 昱光 陈, Jean-Francois Donati, Andrea K. Dupree, Frederick M. Walter, Lynne A. Hillenbrand, Christopher M. Johns-Krull, Carlo F. Manara, Hans Moritz Günther, Min Fang, 敏 房, P. Christian Schneider, Jeff A. Valenti, Silvia H. P. Alencar, Laura Venuti, Juan Manuel Alcalá, Antonio Frasca, Nicole Arulanantham, Jeffrey L. Linsky, Jerome Bouvier, Nancy S. Brickhouse, Nuria Calvet, Catherine C. Espaillat, Justyn Campbell-White, John M. Carpenter, Seok-Jun Chang, Kelle L. Cruz, S. E. Dahm, Jochen Eislöffel, Suzan Edwards, William J. Fischer, Zhen Guo, 震 郭, Thomas Henning, Tao Ji, 涛 纪, Jessy Jose, Joel H. Kastner, Ralf Launhardt, David A. Principe, Connor E. Robinson, Javier Serna, Michal Siwak, Michael F. Sterzik, Shinsuke Takasao
Figure caption: The [O I] λ6300 line luminosity (blue circles from FEROS, black squares from other instruments) varies with a range of almost a factor of 2 on timescales of months. CHIRON spectra are excluded from this analysis.
Paper: What Are the Radial Distributions of Density, Outflow Rates, and Cloud Structures in the M82 Wind?
Authors: Xinfeng Xu, Timothy Heckman, Michitoshi Yoshida, Alaina Henry, Youichi Ohyama
Figure caption: Radial distribution of electron number density (n  e ) for M82's galactic outflows. The gray symbols are the measurements from the [S II] doublet reported in Yoshida et al. (2019) at different slit positions (Figure 1). Their upper limits are shown as arrows. The red curve is the binned n  e  at different radii considering the gray data points. We have adopted survival analyses to include the upper limits. We also show the best-fit power-law as the blue dashed line. See Section 3.1).