adsabs/AstroCLIMB huggingface dataset:
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Left panel: joint posterior distributions of the log(VMR) of CO, H2O, and CH4 from a KPIC HRS retrieval where we directly fit the molecular abundances and assume they are constant across pressure. Right panel: CCFs of a pure CH4 template with (KPIC data—model without CH4) in blue, and the CCF of the CH4 template with (data—model with CH4) in red. The CH4 template is generated with best-fit parameters of the full model with CH4, CO, and H2O and manually setting opacities of CO and H2O to zero. The gray solid line indicates the companion rest frame, and the gray dotted line is the telluric rest frame. The residuals are taken from two spectral orders (2.29–2.41 μm) with stronger CH4 detection.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Posterior distributions for a few key parameters from LRS retrievals of HD 4747 B, using the EddySed model with MgSiO3 clouds (blue: amorphous; red: crystalline), and MgSiO3 + Fe clouds (purple: amorphous, yellow: crystalline). The titles on each histogram show the median and 68% credible interval for the MgSiO3, am model. The results disagree by as much as 3σ, especially in 2D space, and display strong covariance between C/O and [C/H]. The radius retrieved is also generally smaller than predicted by evolutionary models.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Top panel: best-fit cloudy model (EddySed + MgSiO3, am) in blue and random models drawn from the posterior in light orange for an LRS retrieval of HD 4747 B. The best-fit clear model is overplotted in dashed purple, which fits visibly worse from ≈1.0 to 1.2 μm. Bottom panel: the residuals of the cloudy model shown in error bars, along with random draws of the GP models for the residuals in orange.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Random models drawn from the posterior of the baseline LRS retrieval (MgSiO3, am), plotted over a larger wavelength range and color-coded by [C/H], the metallicity. There is a gradient in [C/H] in the L (≈3.4–4.2 μm) and M (≈4.55–4.8 μm) bands, which can be distinguished with a comparable S/N LRS in these bands. The GPI and SPHERE data are shown in black, and we also overplot the photometric data points from Crepp et al. (2016), which are not included in the retrievals but nonetheless agree with our models.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Solid lines: best-fit VMRs of CO, H2O, and CH4 from our baseline HRS retrieval with chemical quenching. Dashed lines: the corresponding VMRs when quenching is turned off (i.e., equilibrium abundances) for the same retrieval. The 1σ quench pressure is indicated by the gray region, and the blue region shows schematically the pressures where our HRS is sensitive. Within the blue region, the relative CO/CH4 ratio can differ by orders of magnitude between the quenched abundances and the equilibrium abundances.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Filled areas: 1σ intervals for the CO, H2O, and CH4 abundances from our KPIC HRS retrieval. Hatched areas: the same for a joint retrieval (HRS + LRS). The retrieved abundances are two to three times higher in the joint retrieval, while the relative abundance ratios between species stays roughly the same (which produces a similar C/O). This highlights the fact that HRS is better at constraining relative abundances than absolute abundances.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: The best-fit P–T profile from our baseline HRS retrieval in blue, with the thicker region indicating the retrieved quench pressure (2σ interval of 14–836 bars). Lines of constant log(CO/CH4) VMRs are shown, with black lines (gray lines) indicating the region where CO (CH4) is more abundant. The P–T profile nearly overlaps with the log(CO/CH4) = +1 line below ∼20 bars, which is where we retrieve the quench pressure to be from the HRS.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Results from a joint fit to host star radial velocity (top left), relative astrometry (top right), and absolute astrometry (bottom panel) for the HD 4747 system. The data together constrain the orbital parameters and mass of both the companion and host star well (Table 1).
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: Objects that have multiple blended BAL components. The differences in gas physical properties can be observed most clearly with Ca II H and K lines where these absorption lines are only found the lower-velocity components with lower log U and log n (right column). For example, we found three BAL components in SDSS J1448+4043 with the lowest-velocity component showing deep Mg I absorption line as well as Ca II H and K absorption lines (plotted in orange). The data (error) is plotted in black (gray), and the best-fitting model is shown in red with the BAL components are overplotted in green and blue with the continuum plotted in dashed tan lines.
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 three composite I/I 0 model spectra are plotted. The left panel shows the median composite I/I 0 model spectrum for the low ﹩-\mathrm{log}U﹩ BALs, and the middle and the right panels show the same model for the medium ﹩-\mathrm{log}U﹩ BALs and high-log U BALs, respectively. The median log R for each group is noted above each panel. The numbers of BAL components used to generate each composite are also noted. The Mg II λ 2796, Fe II λ 2383, and Fe II*λ 2757 transition models are plotted in red, blue, and yellow, respectively. The pink, light blue, and brown shaded areas represent the median absolute deviation for the Mg II λ 2796, Fe II λ 2383, and Fe II*λ 2757 transitions, respectively. The normalized v off was used on the x-axis where 0 represents v off = 0 km s−1, and −1 (or 1 for v off > 0) represents the maximum BAL velocity measured for each I/I 0 model.
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 outflows from the objects that have more than one FeLoBAL feature are plotted with squares, and the rest of the outflows shown by gray dots. The arrows start from the lower-velocity component and end at the higher-velocity component in the same object. Blue and red arrows (labeled by object) represent objects shown in Figures 10 and 11, respectively. The shaded diagonal bars for log R were calculated using the typical range of photoionizing photon flux found in our sample of FeLoBALQs (﹩\mathrm{log}Q\sim 55.5\mbox{--}56.5﹩ [photons s−1]). All of the higher-velocity components have higher-ionization parameter, and the majority of them have higher density compared to the lower-velocity components in the same object. Thus the higher-velocity components are located closer to the central black hole. Four of the higher-velocity components with significantly higher log U are overlapping-trough BALs. 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 eight objects with overlapping troughs are plotted with SDSS J1352+4239 (Choi et al. 2020). All the spectra have been shifted to the reference frame of the main BAL trough. The arrows extend from the estimated center of the Mg II trough to the center of emission line to illustrate the BAL offset velocity. The full spectral models and the continuum models are plotted in red and dashed blue lines, respectively. The green dotted–dashed lines show the unabsorbed line emission and continuum emission if present. The additional blue dashed lines in the three objects on the right column represent the unabsorbed power-law continuum emission. The shaded regions represent various absorption lines and absorption-line classes: red, Mg II; blue, low-excitation Fe II; pink, high-opacity moderate-excitation Fe II; yellow, low-opacity moderate-excitation Fe II. Also see Figure 3.
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: Figure 6 modified to show the distributions of absorption strengths (Section 4.3) of select line transitions predicted using the I/I 0 models. Our results point toward the presence of specific absorption lines as being key diagnostics for the location of the outflow (R). The blue diamonds represent the absorption strengths calculated from best-fitting models. The absorption strengths represented with green diamonds were calculated from the extrapolated SimBAL models (see text). The gray squares represent the BAL components that are not predicted, showing any opacity from the line transition featured in each panel. The size of the diamonds is proportional to values of the absorption strength parameter (i.e., larger markers represent stronger absorption). The Ca II absorption lines are only found in distant BALs (﹩\mathrm{log}R\gtrsim 3﹩ [pc]), and Balmer absorption lines are found in BALs with ﹩\mathrm{log}R\lesssim 1﹩ [pc]. He I* absorption lines are predicted and found in nearly all FeLoBALs. The error bars show 2σ (95.45%) 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: Objects that show multiple outflows where each BAL component (indicated with blue and green model curves) is clearly separated (Mg II λλ2796,2803 troughs are not blended, left column). The data (error) is plotted in black (gray), and the best-fitting model is shown in red with the BAL components overplotted in green and blue. The column on the right shows the wavelength region where He I*, Ca II H, and K absorption lines are found. Note the BALs in these objects have low ionization, and no He I* absorption-lines are observed.
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 correlation coefficients calculated for all measured-BAL property pairs. The size and the color of the markers reflect the values of Kendall’s rank correlation coefficient. The values with asterisks and cyan crosses represent the pairs that showed statistically significant correlations (p < 0.01). The first six parameters (log U, log n, ﹩\mathrm{log}{N}_{H}-\mathrm{log}U﹩, v off, v width, and log a) are the best-fitting model parameters from SimBAL, and the rest are the derived properties calculated from the model parameters.
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 width measurements from different line transitions are plotted with 2σ (95.45%) error bars. The widths measured with the excited-state Fe II are noticeably smaller than the widths measured from the Mg II or the ground-state Fe II transitions. Objects with the excited-state Fe II transition are plotted with orange diamonds.
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: Optical and UV light curves of AT2021ehb. The host contribution has been removed using difference photometry (ZTF, Section 2.1) or subtraction of fluxes estimated from the galaxy SED (Ultra-Violet/Optical Telescope, UVOT; Section 2.4.2). Photometry has only been corrected for Galactic extinction. The transparent lines are simple Gaussian process fits in each filter (see Section 4.1), where the width of the lines represent 1σ model uncertainties. For clarity, we only show the model fits in the r ZTF, uvw1, and uvw2 bands. Regions where the model uncertainty is greater than 0.3 mag are not shown. The lack of ZTF and UVOT data at 0 ≲ δ t ≲ 50 days is due to Sun occultation; The lack ZTF data at 220 ≲ δ t ≲ 290 days and 310 ≲ δ t ≲ 340 days is due to performance issues with the cooling system for the ZTF Camera (Fremling et al. 2021). The lack of UVOT data at 270 ≲ δ t ≲ 300 days is due to an issue with one of the Swift reaction wheels (Cenko 2022).
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: Optical spectroscopic evolution of AT2021ehb. The observed spectra have been corrected for Galactic extinction. The vertical lines mark observed strong host absorption lines and spectral features common in TDEs. The vertical gray bands mark atmospheric telluric features, and strong telluric features have been masked. The best-fit galaxy model is shown at the bottom (see Section 3.2).
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: Evolution of the UV/optical blackbody properties of AT2021ehb compared with a sample of recent X-ray bright TDEs in the literature, including AT2018fyk (Wevers et al. 2019a, 2021), AT2019dsg (Stein et al. 2021), AT2019azh (Hinkle et al. 2021), AT2020ocn, and AT2019ehz (van Velzen et al. 2021). The results of “good epochs” (see definition in the text) are shown in high-opacity colors, whereas results of “ok epochs” are shown in semitransparent.
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: Radio upper limits for AT2021ehb in the context of other UV- and optically discovered TDEs with radio data, including ASASSN-14li (Alexander et al. 2016), ASASSN-15oi (Horesh et al. 2021a), iPTF16fnl (Horesh et al. 2021b), AT2018fyk (Wevers et al. 2019a, 2021), AT2018hyz (Cendes et al. 2022), AT2019azh (Goodwin et al. 2022; Sfaradi et al. 2022), AT2019dsg (Cendes et al. 2021a), and upper limits listed in Table 2 of Alexander et al. (2020).
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: Host galaxy SED of AT2021ehb. The open squares are the Galactic extinction-corrected host photometry (see Table 3). The green lines are samples from the posterior distribution of host galaxy SED models. The open circles are the synthetic host galaxy magnitudes in the observed bands (shown in blue) and in the UV filters of Swift/UVOT (shown in purple).