adsabs/AstroCLIMB huggingface dataset:
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Results of the local simulation with α = 10−5 for λ = 0.25, 1, and 4 au. The blue, green, and yellow solid lines show the evolution of δΣd/Σd ,0 for each wavelength. The gray dotted line shows the time evolution of the background stopping time τ s,0. The blue, green, and yellow dashed lines show the growth rates derived in the previous linear analyses (Equation (18)). We use physical values at times marked by the orange filled circles to derive the growth rate. The linear analyses have a good agreement with each simulation.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Dust surface density profiles around the most collapsed ring in the six runs. We plot filled circles at the cell positions, with color showing the condition for secular GI (see Equation (C1)). Secular GI can operate for 1 − F > 0.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Density and radial speed distributions from the WSA-ENLIL simulation in the ecliptic plane at 01:01:06 UT on 2020 December 1 (top) and 07:00:21 UT on 2020 December 2 (bottom). The values of the density and speed are scaled by the color bar at the right corner of each panel. The positions of the Earth, STEREO A, and PSP are marked by the circle, triangle, and square, respectively. The first time indicates the moment when the CME have just passed PSP and would arrive at STEREO A. The second time is close to the CME arrival time at the Earth.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: In situ solar wind measurements and simulation results at PSP. From top to bottom, the panels show the normalized 314 eV electron PAD, proton density, bulk speed, proton temperature, magnetic field strength, and components, respectively. Note that there are no plasma data from PSP during the time of interest. The red dashed lines represent the simulation results. The blue vertical dashed lines indicate the observed arrival times of the shocks marked with “S0” and “S,” respectively. The shaded regions indicate the intervals of two ICMEs.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Radio dynamic spectra associated with the 2020 November 29 eruption from PSP, STEREO A, and Wind. The white arrows mark the type II radio burst observed by the spacecraft. The shock nose distances derived from the ellipsoid model are converted to frequencies by using the Leblanc density model with an electron density of 15 cm−3 at 1 au. The frequencies are overlapped in the spectra as red crosses. The white curve in the middle panel is the GOES X-ray flux scaled in arbitrary units. The vertical dashed lines represent the shock arrival times from in situ measurements at PSP and STEREO A. The areas with radio bursts are expanded and plotted over each image for clarity.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: In situ solar wind measurements and simulation results at Wind. From top to bottom, the panels show the normalized 265 eV electron PAD, proton density, bulk speed, proton temperature, magnetic field strength, and components, respectively. The red dashed lines represent the simulation results, and the density from the simulation is divided by a factor of 5. The dotted line in the fourth panel denotes the expected proton temperature calculated from the observed speed (Lopez 1987). The black vertical dashed lines indicate the interval of the ICME-like structure.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: In situ solar wind measurements and simulation results at STEREO A. From top to bottom, the panels show the normalized 93–247 eV electron PAD, proton density, bulk speed, proton temperature, magnetic field strength, and components, respectively. The red dashed lines represent the simulation results, and the density from the simulation is divided by a factor of 10. The dotted line in the fourth panel denotes the expected proton temperature calculated from the observed speed (Lopez 1987). The blue vertical dashed line indicates the observed arrival time of the shock marked with “S,” and the shaded region indicates the interval of the ICME.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: Sketch of the projected spatial distribution of the confirmed explosive dispersal outflows (red crosses), plus S106 IR (blue inverted triangle; Bally et al. 2022) in the Milky Way (artist's concept, R. Hurt: NASA/JPLCaltech/Spitzer Science Center). The location of the Sun is marked with the circle at the crossing of the two dashed lines.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: Models (the green curve and shaded region) of good qualitative agreement with an isotropic expansion at constant velocity (V outflow = 83 km s−1) on the PV diagram, setting t dyn = 3500 ± 500 yr.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Our sample of FeLoBAL outflows and the compilation of outflows from Fiore et al. (2017). Left panel: the regression slopes shown as the dotted, dashed, and dotted–dashed lines for the molecular outflows, ionized winds, and X-ray outflows, respectively, taken from Fiore et al. (2017). The green line has a slope of one that represents ﹩{\dot{M}}_{\mathrm{Out}}={\dot{M}}_{\mathrm{Accretion}}﹩ (assuming the energy-conversion efficiency, η = 0.1). The purple line (shade) showing the regression for our sample of FeLoBALs has the slope of 1.02 ± 0.25, which is consistent with both ionized winds (1.29 ± 0.38; dashed line) and X-ray outflows (1.12 ± 0.16; dotted–dashed line). This result is also consistent with ﹩{\dot{M}}_{\mathrm{Out}}/{\dot{M}}_{\mathrm{Accretion}}\sim 3﹩, although we observe a wide range of this ratio from ∼0.04 to ∼80 among the objects in our sample. Right panel: the solid, dashed, and dotted lines show L KE = 1.0, 0.05, 0.005L Bol, respectively. Pink square outlines denote the powerful outflows (L KE/L Bol > 0.005) in our sample that have well-constrained physical parameters and outflow properties. The red cross represents the outflow in SDSS J1352+4239 (Choi et al. 2020). The vertical error bars show 2σ (95.45%) uncertainties.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption:  Left panel: the physical parameter distribution of intervening absorbers cannot be easily differentiated from that of FeLoBAL. Middle panel: intervening absorbers have low densities, and we were able to constrain only the density upper limits (﹩\mathrm{log}n\lesssim 2.8\,[{\mathrm{cm}}^{-3}]﹩) for the majority of them. Based on the ionization parameter and the density, we found the inferred distances from the central engine to the intervening absorber gas to be ﹩\mathrm{log}R\gtrsim 3﹩ [pc], if we assume the radiation from AGN as the ionizing source for these absorbers. Right panel: the kinematic properties show the clearest distinction between the intervening absorbers and FeLoBALs. The intervening absorbers have very narrow width (v width ≲ 200 km s−1) and disproportionately large offset velocities (v off ≪ − 3, 000 km s−1), relative to the quasar rest frame, compared to FeLoBALs. The brown dotted–dashed line shows a one-to-one ratio. We rejected SDSS J1057+6109 (green diamonds) from the analysis because the properties of the absorption feature seen in the spectra better resembled the intervening absorbers than the quasar-driven outflows (Section 3.3.1). A linear scale was used in the region ∣v off∣ < 100 km s−1, and log scale was used elsewhere in the x-axis. The error bars show 95% uncertainties, and the gray shaded bars represent the range of the values among the tophat model bins for each BAL.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The distributions of the offset velocities (v off) and the distances of the BALs from the central SMBHs (log R). The blue shaded region represents the defining criteria for the loitering outflows (﹩\mathrm{log}R\lt 1,| {v}_{\mathrm{off},\mathrm{FeII}\,\mathrm{excited}}| \,\lt 2000\,\mathrm{km}\ {{\rm{s}}}^{-1}﹩, and v  width,FeII excited < 2000 km s−1). Excluding the loitering outflows and the inflows (v off > 0), we found robust statistical evidence (p < 0.05) for a correlation between log R and v off where the high-velocity flows are found closer to the central engine. The error bars show 2σ (95.45%) uncertainties.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The outflow velocity (v off) is plotted against the SED slope parameter (α  ui ). FeLoBALs with higher outflow velocities are found in objects with flatter or redder SEDs, where FeLoBALQs with steeper or bluer SEDs have compact outflows (﹩\mathrm{log}R\lesssim 1﹩ [pc]). Most of the compact outflows with steep SEDs are loitering outflows, and α  ui  in these objects might be potentially affected by other SED properties than reddening such as the strength of IR emission from the torus (K. M. Leighly et al. 2022, in preparation). The top axis shows the values of E(B − V) that correspond to the range of α  ui  plotted on the bottom axis (assuming a composite quasar SED (Richards et al. 2006) and SMC reddening (Prevot et al. 1984)). The vertical error bars show 2σ (95.45%) uncertainties.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The force multiplier (FM) calculated using Cloudy with physical parameters from the best-fitting SimBAL models. Left panel: the FM is strongly correlated with ionization parameter. Right panel: we did not find robust correlation between the FM and the outflow velocity. The outflows with the highest-outflow velocities have relatively smaller FM. An extra source of opacity to capture the photon momentum, such as dust, or other acceleration mechanisms, may be needed to explain the high-velocity FeLoBALs. The high values of α  ui , flat or red SEDs, found in these objects could potentially indicate dusty outflows. Markers and error bars as in Figure 4.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The summary of FeLoBAL properties found in our sample.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption:  Left panel: the bolometric luminosity as a function of outflow velocity. The gray points represent the compilation of outflows from Fiore et al. (2017), and the red cross shows the FeLoBAL outflow in SDSS J1352+4239 (Choi et al. 2020). The purple line represents the regression slope, ﹩{L}_{\mathrm{Bol}}\propto {v}_{\mathrm{off}}^{0.5}﹩, for our sample of FeLoBAL outflows, which differs dramatically from the ﹩{L}_{\mathrm{Bol}}\propto {v}_{\mathrm{off}}^{5}﹩ scaling (dashed gray lines) described in Fiore et al. (2017). Right panel: the momentum flux ratio (﹩{\dot{P}}_{\mathrm{outflow}}/{\dot{P}}_{\mathrm{AGN}}﹩) as a function of outflow velocity. The dashed horizontal line marks the expected ratio for a momentum conserving outflow. The error bars show 95% uncertainties.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The mean spectra corresponding to our five principal sets of eigenvectors for near-UV model fitting. The five subsamples were constructed using k-means clustering on the first four EMPCA eigenvector reconstruction coefficients from analysis of the whole sample. The five sets of eigenvectors (plus an extreme Fe II/Mg II set) are sufficient to model most near-UV line emission morphologies.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: The spectrum of the second joint NICER and NuSTAR observations (2022 January). See Table 5 for best-fit parameters. NuSTAR/FPMB and NICER data have been divided by C FPMB and C NICER, respectively. The data have been rebinned for visual clarity. In the lower-left panel, we also show the reflection contribution and the direct PL contribution individually from relxill. In the lower-right panel, we also show the best-fit model (2d) deconvolved with the xstar component.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Upper: UV (uvw1UVOT) and optical (r ZTF) light curves of AT2021ehb. Middle: XRT and NICER X-ray net count rates of AT2021ehb. Epochs of XMM-Newton, SRG, and NuSTAR observations are marked by the vertical lines. Lower: XRT and NICER hardness ratio (HR) evolution of AT2021ehb.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Long-slit optical spectra of AT2021ehb taken at eight different epochs. The spectrum (f  λ,obs) is plotted in black. The blackbody continuum (A 1 f  λ,BB ;  dotted lines) plus host galaxy spectrum (A 2 f  λ,host) is plotted in green. No spectral features commonly seen in optically selected TDEs are observed in AT2021ehb.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Best-fit incident model spectra of (2c) and (2d), as well as modifications of (2c) if one parameter is changed.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: The spectrum of the second joint NICER and NuSTAR observations (2022 January). This figure highlights the flux levels of the source and background spectra.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: The spectrum of the first joint NICER and NuSTAR observations (2021 November). See Table 4 for best-fit parameters. NuSTAR/FPMB and NICER data have been divided by C FPMB and C NICER, respectively. The data have been rebinned for visual clarity.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: The XMM-Newton spectra. The data have been rebinned for visual clarity. The dashed lines show the best-fit models. See Table 6 for the best-fit parameters.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: XRT time-averaged spectra of AT2021ehb. See the lower panel of Figure 8 for the time span of each spectrum.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: SRG/eROSITA spectra of AT2021ehb.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Comparisons of our EC 53 model light curves for the SMA (left column) and JCMT (right column), with variations in the envelope parameters. The fiducial model is marked in each panel by the blue line, and the origin on the time denotes the peak brightness of the source (see Figure 7). The triangles show the peak position for each curve. The varied parameters are as follows: first row: envelope floor temperature T floor; second row: envelope density power-law index α; third row: envelope outer radius r out; and fourth row: envelope inner radius r in.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Light curves for the variable targets observed with the ACA (large green circles) and contemporaneous JCMT 850 μm observations (small blue circles). The ACA flux measurements are shown after relative calibration (Section 3.1) has been applied. The JCMT data for each source have been scaled such that the mean light-curve flux is equal to the mean of the ACA data (dashed black line).