adsabs/AstroCLIMB huggingface dataset:
Paper: Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Authors: Tomoko L. Suzuki, Karl Glazebrook, Corentin Schreiber, Tadayuki Kodama, Glenn G. Kacprzak, Roger Leiton, Themiya Nanayakkara, Pascal A. Oesch, Casey Papovich, Lee Spitler, Caroline M. S. Straatman, Kim-Vy Tran, Tao Wang
Figure caption: (Left) Continuum flux at ∼870 μm as a function of stellar mass of our targets. For comparison, we show galaxies with individual Band 7 detections at z = 3–4 from the literature (AS2UDS: Dudzevičiūtė et al. 2020; A3COSMOS: Liu et al. 2019) and quiescent galaxies at z = 3–5 with Band 7 data (Santini et al. 2019). The four quiescent galaxies in this work are fainter at submillimeter wavelengths by ≳1 dex than the SMGs at z = 3–4. (Right) SFRIR as a function of stellar mass of our targets together with quiescent galaxies at z = 3–5 with Band 7 and/or 6 data from Santini et al. (2019). We show the SFRs estimated with both T dust = 40 K and 20 K for each source except for Hyde. The data points with the lower SFRs represent the results assuming T dust = 20 K. The black solid line shows the main sequence of star-forming galaxies at z = 3.7 from Speagle et al. (2014). The dashed–dotted line shows the star-forming main sequence at z = 3.7 from Tomczak et al. (2016), which is established with the ZFOURGE galaxy catalog. The four quiescent galaxies including ZF-COS-19589 with the continuum detection have more than four times lower SFRs than the main-sequence galaxies even when assuming the higher T dust. All the upper limits are 3σ upper limits.
Paper: Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Authors: Tomoko L. Suzuki, Karl Glazebrook, Corentin Schreiber, Tadayuki Kodama, Glenn G. Kacprzak, Roger Leiton, Themiya Nanayakkara, Pascal A. Oesch, Casey Papovich, Lee Spitler, Caroline M. S. Straatman, Kim-Vy Tran, Tao Wang
Figure caption: Relation between stellar mass and the molecular gas-mass fraction upper limit of our targets. Here we show the stacking result for all five galaxies. We also show quiescent galaxies at z = 1−3 from the literature (Sargent et al. 2015; Belli et al. 2021; Caliendo et al. 2021; Magdis et al. 2021; Williams et al. 2021) for comparison. The solid line shows the scaling relation between M * and f gas for galaxies on the star-forming main sequence at z = 3.7 from Tacconi et al. (2018). The two dashed lines represent the scaling relations when the galaxies are located 5× and 10× below the main sequence. Our individual galaxies and the stacking result at z = 3.5–4.0 have more than 3 times lower molecular gas-mass fractions as compared to the scaling relation for the main-sequence galaxies at z = 3.7.
Paper: Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Authors: Tomoko L. Suzuki, Karl Glazebrook, Corentin Schreiber, Tadayuki Kodama, Glenn G. Kacprzak, Roger Leiton, Themiya Nanayakkara, Pascal A. Oesch, Casey Papovich, Lee Spitler, Caroline M. S. Straatman, Kim-Vy Tran, Tao Wang
Figure caption: Gas-mass fraction of quiescent galaxies obtained by this study and previous studies (Sargent et al. 2015; Spilker et al. 2018; Davis et al. 2019; Belli et al. 2021; Caliendo et al. 2021; Magdis et al. 2021; Williams et al. 2021) as a function of redshift. The thick solid line represents the evolution of gas-mass fraction for star-forming galaxies on the main sequence with ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=10.8﹩ from Tacconi et al. (2018). The shaded area corresponds to the scatter of the main-sequence relation (0.3 dex). The red dashed line shows the evolution of gas-mass fraction of the quiescent galaxies at z ∼ 3.7 when assuming the closed-box model and gas depletion timescales of 0.4 and 2.4 Gyr.
Paper: Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Authors: Tomoko L. Suzuki, Karl Glazebrook, Corentin Schreiber, Tadayuki Kodama, Glenn G. Kacprzak, Roger Leiton, Themiya Nanayakkara, Pascal A. Oesch, Casey Papovich, Lee Spitler, Caroline M. S. Straatman, Kim-Vy Tran, Tao Wang
Figure caption: ALMA Band 7 and HST/F160W images of all the targets (image size: 3″ × 3″). The blue and magenta plus marks show the coordinates from the ZFOURGE catalog (Straatman et al. 2016) and the position of the 870 μm flux peak (when detected), respectively. The black filled circle in each ALMA map represents the beam size.
Paper: Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Authors: Tomoko L. Suzuki, Karl Glazebrook, Corentin Schreiber, Tadayuki Kodama, Glenn G. Kacprzak, Roger Leiton, Themiya Nanayakkara, Pascal A. Oesch, Casey Papovich, Lee Spitler, Caroline M. S. Straatman, Kim-Vy Tran, Tao Wang
Figure caption: 1D spectrum around the [C I] line extracted at the position from the ZFOURGE catalog of each target. The velocity binning size is 100 km s−1. The red dashed line in each panel corresponds to the frequency of the redshifted [C I] line. We found no emission line feature with >3σ  at the observed frequency of [C I].
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Crab spectrum before (left) and after (right) the inclusion of the negative Si edge. There are initially strong residuals around 1.8 keV. After the inclusion of a negative Si edge, the residuals around 1.8 keV are greatly improved.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Schematic approximate location of various galactic structures in the E − L  z  space adopted from Naidu et al. (2020). The approximate location of our Atari disk sample is highlighted by the blue ellipsoid. Our Atari disk sample overlaps with the E − L  z  space of the Wukong, the in situ halo, and the α-rich disk (canonical thick disk).
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Orbital eccentricity distribution for our Atari disk sample, using the scale length of h  R  = 2.48 ± 0.15 kpc and scale height of h  Z  = 1.67 ± 0.15 kpc in the ranges of 1 < ∣Z/h  Z ∣ < 3 and 2 < ∣R/h  R ∣ < 3, corresponding to Figure 3 in Sales et al. (2009). The solid black line represents the superposition of the individual Gaussians. Top panel: best fit using two Gaussians with peaks at e = 0.30 and 0.49. Bottom panel: best fit using three Gaussians with peaks at e = 0.16, 0.33, and 0.51.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Top: orbital eccentricities as a function of [Fe/H] with a gradient of ∂e/∂[Fe/H] = − 0.05 ± 0.01 dex−1. Bottom left: e as a function of the Galactocentric radial distance R with a flat trend of ∂e/∂R = 0.00 ± 0.00 kpc−1. Bottom right: e as a function of scale height Z with a positive gradient of ∂e/∂∣z∣ = + 0.01 ±0.002 kpc−1. Error bars denote the standard deviation throughout.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Top: MDF for stars with [Fe/H] < −0.8 of the action selected method (gray histogram), the velocity selection method (red histogram), and our Atari disk sample (green histogram). The inset figure shows the MDFs of stars with [Fe/H] < −2.5 and the best-fitting exponential (﹩{\rm{\Delta }}\mathrm{log}{\text{}}N/{\rm{\Delta }}[\mathrm{Fe}/{\rm{H}}]=1.13\pm 0.06﹩). Bottom: MDF of the metal-poor tail (with [Fe/H] < −2.5) of our Atari disk sample (green histogram) compared with the sample of stars that we identify as Atari disk stars from JINAbase (blue histogram).
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: Formation and evolution of representative intermediate-period and long-period sdBs from the zero-age main sequence (ZAMS) to the final WD cooling stage in the H-R diagram. The solid lines denote the evolutionary tracks and the corresponding colors (as given by the color bar) indicate the percentage of the combined ideal gas and electron degeneracy pressures that is solely due to degeneracy (evaluated at the center). A filled circle denotes the start of a mass-transfer phase and a triangle denotes the end of that phase. The ZAMS progenitor star for the intermediate-period case has a mass of 3.5 M ⊙ and an approximately solar metallicity (Z = 0.02). Mass transfer is initiated in the Hertzsprung gap and continues as the progenitor ascends the red giant branch (denoted as RGB). Mass transfer ceases once its mass is reduced to 0.47 M ⊙, and this stripped core evolves along the horizontal branch until it reaches the sdB phase. This phase (annotated and denoted by the black dashed lines overlaid on the evolution curves) persists for almost 80 Myr before the hot subdwarf subsequently evolves through the sdO phase (distinguished by the brown dashed lines) for an additional 40 Myr. The evolution of the companion star is also shown; its initial mass is 1.6 M ⊙, and it undergoes a phase of rapid accretion before it reaches thermal equilibrium (after mass transfer has ceased) and evolves normally as a 1.9 M ⊙ star. The star ascends the RGB, and the evolution is halted once the star is large enough to fill its Roche lobe. The progenitor star of the long-period sdB binary has a primordial mass of 1.2 M ⊙ and evolves up the RGB until it is close to its tip, at which point it starts to lose mass rapidly. After a series of thermal adjustments, it enters the sdB phase, which persists for ≈75 Myr (annotated); for reasons of clarity, the evolution of its companion is not shown. Note that the observable properties of the sdBs in both the intermediate- and long-period scenarios are quite similar, as are the fractions of electron degeneracy pressure in both stars during most of their sdB and sdO phases.
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: SED plot for TIC 5724661 (black points), where the smooth curves are the model fits using Kurucz & Castelli model atmospheres (Castelli & Kurucz 2004) for the sum of the A star and the inferred sdB star; these have been corrected for interstellar extinction. The fits are described in detail in the text. The green curve is for the A star alone, while the orange curve represents the flux of a companion sdB star. It is evident that the sum of the models for an A star and an sdB star can explain the observed SED much better than either would on its own. This lends credence to our claim that there is a compact, hot body orbiting the A star.
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: Evolution of the bolometric luminosity, individual nuclear luminosities, and radius of the representative hot subdwarf as a function of time. Note that t * = 0 has been chosen to approximately coincide with the end of the RGB phase (t * = t − 211.25 Myr). The sdB phase persists for nearly 80 Myr, during which time helium is continuously depleted due to triple-α burning and the fusion of carbon into oxygen (α-channel burning). Once a CO core forms and the subdwarf experiences He-shell flashes, it enters into a shorter-lived sdO phase. For each phase, the radius of the subdwarf is approximately constant.
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: The evolution of the orbital period as a function of the mass of the primary (i.e., the sdB star’s progenitor). Representative binaries for both the intermediate- and low-mass cases are shown. The respective initial masses of the primary and the secondary (in solar units) and the value of β for each of the three sets of curves are listed in the diagram. For the black curves, the initial orbital periods are 2.2, 2.8, 3.4, and 4.0 days (solid, dotted, dashed, and dashed–dotted lines, respectively) and for the blue curves, the initial periods are 2.6, 3.5, 4.4, and 5.3 days (solid, dotted, dashed, dashed–dotted lines, respectively). For the low-mass cases (red curves), the initial orbital periods are 280, 300, 320, 340, and 400 days (solid, dotted, dashed, dashed–dotted, and long-dashed lines, respectively). The “canonical” range of masses for sdB stars (0.45–0.47 M ⊙) is denoted by the two vertical dashed lines.
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: Plots showing how various properties of the sdB components of two representative binaries correlate with their respective initial periods, for two intermediate-mass cases. The dark green dots correspond to a system in which the initial mass of the sdB star’s progenitor was 3.25 M ⊙, its companion’s initial mass was 1.7 M ⊙, and β was fixed at 0.95. The purple diamonds correspond to a system in which the initial mass of the sdB star’s progenitor was 3.5 M ⊙, its companion’s initial mass was 1.6 M ⊙, and β was fixed at 0.9. The plots show that for longer initial periods, the sdB star’s final period, mass, radius, and luminosity increase; however, its effective temperature and ﹩\mathrm{log}g﹩ decrease. These trends remain robust even when the initial masses are changed. Note that we have employed a time-average for all parameters whose values change (e.g., the luminosity) during the sdB phase.
Paper: TIC 5724661: A Long-period Binary with a Pulsating sdB Star and δ Scuti Variable
Authors: Rahul Jayaraman, Saul A. Rappaport, Lorne Nelson, Donald W. Kurtz, George Dufresne, Gerald Handler, Abdel Senhadji, David W. Latham, George Zhou, Allyson Bieryla, George R. Ricker
Figure caption: Posterior distributions for the parameters of TIC 5724661. This corner plot shows the best-fit parameters and the correlations between the parameters derived through an MCMC fitting code. Dashed vertical lines, from left to right, represent the 16th percentile, median, and 84th percentile. The distribution for the temperature of the sdB star seems to fall off at high temperatures, suggesting that T eff close to 29,000 K is most likely. There exists a strong degeneracy between T eff and the radius of the sdB star, as expected given the limited region of the SED where the sdB star likely dominates the system light.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: How to measure the width of a CME. The four consecutive frames of the CME illustrate the evolution of the width of the CME on 2014 May 6 17:36:05 UT. The red arrows indicate the upper and lower edges of the CME intersecting with the occulting disk. The blue arrow corresponds to the leading edge of the CME. The data output from the measurement tool are given below the images.
Paper: Effect of the Heliospheric State on CME Evolution
Authors: Fithanegest Kassa Dagnew, Nat Gopalswamy, Solomon Belay Tessema, Sachiko Akiyama, Seiji Yashiro
Figure caption: The transition height (hc) of an SC 23 CME (left) and an SC 24 CME (right) determined from the width vs. height plots. The CME dates, appearance times, and hc values are stated in each plot.
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: Predicted vs. observed W  λ (Lyα) for the LAE sample in Figure 16. We computed the first moment and square root of the second moment of each N = 5 distribution in Figure 16 for the predicted values and their error bars. A right-pointing arrow indicates the predicted value of object z7_GND_34204. A one-to-one dashed line is drawn to guide the eye, and points above this line (the region shaded red) could be the result of IGM absorption.
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: All HST F160W (H-band) images of LAEs in the sample. Each cutout shows a 5″ × 5″ image centered on each galaxy in our sample. The galaxy centroid is indicated with a pink diamond, and the HETDEX detection position and PSF FWHM are indicated by a light-blue cross and dashed circle, respectively. We also include object IDs and redshifts with text.
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: All emission-line detections from the HETDEX survey for LAEs in the sample. The observed data are indicated by the blue lines with gray error bars. A Gaussian model fit to the data is shown in green. The x-axis is scaled in angstroms relative to the line center. Detection IDs and Lyα line redshifts are indicated with text.
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: Comparison of galaxy properties as measured using our “fiducial” model (light blue) vs. our “alternate” model (sea green). The 16th, 50th, and 84th percentiles calculated using the alternate model are indicated by vertical dashed gray lines, and their values are indicated with text. The distributions are consistent, save for dust extinction (AV ), which has lower values by a factor of ∼2 for the alternate model.
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: Comparison of correlations between W  λ (Lyα) and galaxy properties as measured using our “fiducial” model (light blue) vs. our “alternate” model (sea green). Binned values from the alternate model are indicated as open gold circles. The correlations presented in Section 4.3 appear robust when different models are adopted.
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: All SED fits for LAEs in the sample (see Figure 9 for a description of the plots). The χ 2 value for each fit is also given with text.
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: Contours of the χ 2 values of each fit. Dark green means large χ 2. Red plus signs indicate the best-fit locations. Top: degeneracy between ﹩\dot{M}﹩ and A  V , with other parameters invariant as in Table 4. Bottom: degeneracy between ﹩\dot{M}﹩ and M *. R * and T 0 (kept equal to T *) are changed along with M * via 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: Model spectra of different accretion rates. Spectral fluxes are not shifted. The four shaded regions in the leftmost panel correspond to absorption lines in the right panels. While the total luminosity substantially changes with ﹩\dot{M}﹩, specific line features such as Mg I, Fe I, and CO lines are nearly unchanged where ﹩\dot{M}\gtrsim {10}^{-6}\ {M}_{\odot }﹩yr−1. Lower accretion rates show gradual transition from disk to photospheric line features. Other parameters are held constant, with M * = 0.3 M ⊙, i = 45°, T 0 = 3400 K, and 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: A small segment of model spectra of different stellar masses, with the product ﹩{M}_{* }\dot{M}=3.0\,\times \,{10}^{-6}{{M}_{\odot }}^{2}﹩ yr−1, i = 45°, A  V  = 10 mag all held constant, and T 0 set as the minimal value of T * given by the PMS model. The spectra are vertically shifted. They do not perfectly overlap before the offset because T visc also depends on R in in Equation (1). The two Fe I lines show that higher M * entails broader, shallower profiles. Some thin needle-shaped lines are present in the M * = 1.20 M ⊙ spectrum; they originate from higher photospheric luminosity predicted by the standard PMS model.