adsabs/AstroCLIMB huggingface dataset:
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: CSM density profiles resulting from the eruption (left) and wind (right) mass-loss models. The gray lines in the left (right) panel show the corresponding ejecta masses (mass-loss rates) of ﹩{M}_{\mathrm{ej}}(\dot{M})=0.1﹩, 1, and 10 M ⊙ (M ⊙ yr−1). For the same event, different points are calculated by different velocities obtained by observations (see Table 1).
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Top panel: N H,24μm vs. L IR(8–1000 μm). Bottom panel: N H(8 × 8 pc2) vs. L IR(8–1000 μm) We assumed z = 2.0, and the plots were observed from θ = 0°. The color bar represents the Eddington ratio. The plus signs do not satisfy the DOG criteria. Squares indicate bump DOGs and triangles indicate PL DOGs.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Time evolution of the system in the two-color diagram (z = 2.0). The AGN wedge is represented in gray (Mateos et al. 2012). The plus signs do not satisfy the DOGs criteria. The meanings of the plus, square, and triangle symbols are the same as in Figure 9. Top panel: θ = 0°, bottom panel: θ = 60°.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: DOG-type evolution for θ = 0° with varying AGN feedback efficiency (η AGN). In the top panel, η AGN is 0.8%; in the bottom panel, η AGN is 2.0%.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Intensity distribution in the optical to mid-infrared for θ = 90° at t = 1107.0 Myr.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Map of column density projected to the x–y plane at t = 1103.3 Myr (top panel) and 1107.0 Myr (bottom panel).
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Scatter plots between the CME speeds and the heights of constant width of limb CMEs in SC 23 (red) and SC 24 (blue). There are only 562 CMEs in SC 23. The 34 CMEs whose actual hw values are difficult to measure were dropped. The slope of the regression line in SC 24 is 168% higher than that in SC 23. The data used to create this figure are available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Scatter plots between the CME speeds and the heights of constant width. There are 596 CMEs in SC 23. Interpolation/extrapolation is used to estimate the actual hw values of the 34 CMEs. The slope of the regression line in SC 24 is 111% higher than that in SC 23. The data used to create this figure are available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Scatter plots between the CME speeds and transition heights of 1002 limb CMEs in SC 23 (red) and SC 24 (blue). The red and blue solid lines signify linear fits to the data points. The slope of the regression lines and the corresponding equations along with the correlation coefficients are shown in the plots. Note the distinct regions occupied by the SC 23 and SC 24 data points on the plots. The data used to create this figure are available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Comparison of the transition heights between the corresponding phases of SC 23 and SC 24. The red (top row) and blue (bottom row) histograms correspond to the number of limb CMEs vs. transition height for the rise, maximum, and decline phases of SC 23 and SC 24, respectively. The numbers of limb CMEs in the rising phase (left-hand panels), maximum phase (middle panels), and declining phase (right-hand panels) along with the corresponding mean and median values are stated on the panels. These figures can be reproduced using the data available in the machine-readable formats of Table 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Comparison of the transition heights (hc) between SC 23 and SC 24. The red (SC 23) and blue (SC 24) histograms denote the number of limb CMEs with corresponding transition heights. The number of CMEs, the corresponding mean, median, and standard error of the mean values are specified in each plot. The average value of hc in SC 24 is larger than in SC 23. The data used to create these figures are available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Size distributions of GOES soft X-ray flares associated with CMEs in SC 23 (left) and SC 24 (right). The number of limb CMEs and the mean and median values of the X-ray flare sizes of each cycle are stated on the panels. These figures can be reproduced using the data available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Comparison of speeds of limb CMEs in SCs 23 (left) and 24 (right). The number of limb CMEs and the corresponding mean and median CME speeds are stated in each plot. These figures can be reproduced using the data available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Variations of hc over time for the corresponding phases of SC 23 (left) and SC 24 (right). The green, red, and blue circles refer to the rising, maximum, and declining phases in both cycles. The data used to create these figures are available in the machine-readable formats of Tables 1 and 2.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: Transition heights as a function of CME dates showing the time variations of 600 limb CMEs in SC 23 (left) and 406 limb CMEs in SC 24 (right). These figures can be reproduced using the data available in the machine-readable formats of Tables 1 and 2.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The relationship between W  λ (Lyα) and (clockwise from top left) stellar mass, SFR, sSFR, dust extinction (A V ), mass-weighted age, and UV slope (β) for all objects in the sample. Gray lines indicate the ±1σ error bars on physical properties and equivalent width. Open red circles show medians and standard deviations for properties in equivalent width bins having equal numbers of objects. Pearson correlation coefficients, r  p , and p-values are indicated for each plot. Stellar mass and SFR exhibit the strongest correlations with W  λ (Lyα), while age and sSFR correlate moderately. Surprisingly, no strong correlation exists with dust extinction.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: Probabilistic predictions of W  λ (Lyα) for 10 LAEs at z > 7 having emission-line S/N > 4. The distributions were normalized by setting their integrals to unity. We chose stellar mass, SFR, and dust extinction as predictive properties for this calculation. Gold, magenta, and indigo lines show the probability distribution of our predictions using N = 3, 5, and 7 nearest neighbors, and the gray shaded region shows the 68% confidence interval for the equivalent width measurements from Jung et al. (2020). Object IDs and redshifts are indicated with text for each plot. We find good agreement between prediction and observation for the majority of strong emitters.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: Left: an example fit to the SED of an LAE in the sample. Data are shown by blue circles, and the 68% spread for the posterior model photometry and spectrum are shown by the green rectangles and orange shaded lines, respectively. A maroon open circle indicates the measured flux for a filter masked during SED fitting. In this case, the B band was masked out since it includes the Lyα emission line. Our imaging data constrain the 4000 Å break and rest-optical colors. Top right: 5″ square image cutout for the source in the F160W HST filter. The pink cross indicates the source position, and the blue plus sign and dashed blue circle indicate the detection position and the FWHM of the HETDEX fiber PSF. Bottom right: 1D extracted spectrum for this source, centered on an 80 Å window around the Lyα emission line. The solid green line indicates the HETDEX Gaussian model fit to the data.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: A “corner” plot of the fit in Figure 9 for object ID 10388. The 1D histograms are shown on the diagonal for the posterior distribution of each free parameter in our model (see Table 1). The 2D histograms show the correlations of all parameters with one another, where contour lines are drawn for each σ level. With our broadband photometry, we constrained ages, masses, and dust extinctions well.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: (a) The 2D distribution (in S/N and separation space) for objects identified as the imaging counterparts for emission-line detections and those that happened to be spatially coincident. (b) Same as panel (a), but in SED χ 2 and separation space. These two figures show substantial overlap in these parameter spaces for true LAEs and neighboring sources, motivating the benefits of detailed visual inspection shown in Figure 6.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The stellar mass–SFR correlation for LAEs in our sample. The trend fit by Sanders et al. (2018) for z ∼ 2.3 SFGs is drawn in dashed purple for comparison. LAEs in our sample largely fall on the SFMS, though the lowest-mass sources (M ⋆ < 109 M ⊙) tend to fall below the relation.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The equivalent width distribution of LAEs in the sample. An exponential distribution with W 0 = 100 Å is drawn in red for comparison, as well as models fit by Gronwall et al. (2007) and Santos et al. (2020). Our data favor models with larger values of W 0 to best match the number of high-EW sources.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The distributions of posterior median values for (clockwise from top left) stellar mass, SFR, sSFR, dust extinction (in V-band mag), mass-weighted age, and UV slope for all objects in the sample. The 16th, 50th, and 84th percentiles are indicated by vertical dashed gray lines, and their values are indicated with text in the same units as the x-axis labels. The LAEs in our sample exhibit average properties similar to other LAE samples compiled at comparable redshifts using NB selection.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: An example BAGPIPES SED fit for LAE ID z7_GND_42912 at z = 7.51 detected by Jung et al. (2020). For scaling purposes, we do not show the upper limits for nondetections in the HST bands blueward of the Lyα break. From our photometric data, we constrained the stellar population properties of 10 LAEs in the EoR, allowing us to predict their intrinsic Lyα emission using our HETDEX sample.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: CMD in the optical. Left: Model isomass curves through the parameter space. Series of points with the same color but different sizes and markers represent different masses (from 0.1 M ⊙ to 3.0 M ⊙). Black and red dashes respectively mark the transition line and the sufficient dominance line, which separate the isomass curves into three sections: η < 1 (dotted), 1 < η < 5 (dashed), and η > 5 (solid). These three sections agree with the apparent segments of the curves except for the sufficient dominance at M * = 0.1 M ⊙. Extinction is set at A  V  = 10 mag. Right: Comparison of model and observation. M * = 0.3 M ⊙ is fixed for the isomass curves, while extinction varies from 0 to 10. Photometry from Audard et al. (2014) (FUors; red crosses) and Dunham et al. (2015) (YSOs; blue dots) are scaled to d * = 10 pc (see text). The names of the FUors in Section 4.2 plus those specifically discussed in Section 5.2 are annotated. The in-box plot is an overview of the M * = 0.3 M ⊙, A  V  = 10 curve, with three segments corresponding to three η intervals.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Left three: examples of triangle-shaped SEDs at λ = 1.68 μm for a range of accretion rates and extinction A  V  = 10 mag. The sub-panels show a range of accretion rates for specific stellar masses (0.1 M ⊙, 0.6 M ⊙, and 1.8 M ⊙, respectively). Dashed vertical lines indicate the peak of the triangle (F 1, 1.68 μm) and the dotted lines F 2 (1.53) and F 3 (1.78 μm). Right: bolometric flux and the color index Δ = 2F 1/(F 2 + F 3) of model objects with different masses and accretion rates. The three specific fluxes are measured at wavelengths λ = 1.68 μm, 1.53 μm, and 1.78 μm, respectively. Black and red dashes respectively mark the transition line and the sufficient dominance line, which separate the isomass curves into three segments: η < 1 (dotted), 1 < η < 5 (dashed), and η > 5 (solid). The names of the FUors in Section 4.2 are indicated and annotated in red. Extinction is set at A  V  = 10 mag.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Comparison of summed H- and K-band fluxes between the viscous disk and the photosphere with different stellar masses and accretion rates. Filled colors indicate the ratio of flux of the viscous disk to that of the photosphere (η) for a given mass in a logarithmic scale. The black solid line (“transition line”) shows where the two fluxes become equal (η = 1); the red line (“sufficient dominance line”) shows where η = 5. The black dashed line shows where R in = R *. Other parameters are held constant at i = 45°, A  V  = 10 mag, and T 0 as the minimal value T * given by the PMS model.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Mid-IR CMD with WISE W 1 –W 2 color. In the right panel, the black and red dashed lines show the transition line (η = 1) and the sufficient dominance line (η = 5). The names of the FUors in Section 4.2 plus those specifically discussed in Section 5.3 are annotated. For other details, see the caption of Figure 15.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Light curves of the WISE W 1 and Gaia G bands with different starting radii (left: R start = 0.07 au; right: R start = 1.00 au). The two panels share the y-axis. Intervals, marked in red, are measured from ΔW 1 = −1.00 mag through ΔG = −1.25 mag. Black dashed lines denote when the propagation reaches the disk inner boundary.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Left: the EW of CO versus that of Na+Ca for the model objects of various masses and accretion rates and extinction set at A  V  = 10 mag. The colors represent different accretion rates. Shapes of points mark different masses. The gray dashed line is the separation of FUors from other YSOs proposed by CR18. The names of FUors in Section 4.2 are indicated and annotated in magenta. The inset panel is an enlargement of the high-﹩\dot{M}﹩ cluster. Right: normalized Na I, Ca I, and CO absorption lines for ﹩\dot{M}=1\,\times \,{10}^{-6}{M}_{\odot }﹩ yr−1 from the multicomponent models.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Example (M = 0.3 M ⊙) contour plot of the color index Δ as a function of ﹩\dot{M}﹩ (x-axis) and A  V  (y-axis). Black and red vertical lines indicate the transition line and the sufficient dominance line, respectively.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: CMD of HBC 722 at optical and near-IR wavelengths. The black lines indicate model colors and magnitudes with annotated accretion rates. The colored points show published photometries.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Observed data and best-fit model of the SEDs of HBC 722 in the optical. This is an enlargement of Figure 9 (bottom left).
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: A graphic illustration of the possible 3D configuration that gives raise to the observed structure in Figure 10. A filamentary structure seen in N2H+ (1–0) emission accretes material toward protostellar core p2. This launches a bipolar outflow likely almost perpendicularly to the accretion flow. The red lobe, when projected on the plane of the sky, appears to coincide with the filament.