adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: The sgscore1 (star–galaxy classification score) and magnr (magnitude of the nearest object in the ZTF reference image) parameters of 55 photometric TDE candidates. Symbol colors follow the same convention as in Figure 2. The 33 TDEs are shown in solid markers, and the 22 false positives are shown in hollow markers. We show the ZTF names for objects with sgscore1>0.2.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Host galaxy SEDs (sorted by redshift). The gray and black squares show the observed and Galactic extinction-corrected photometry, respectively. The blue lines show models of the 100 walkers in the MCMC sampler. The dotted and dashed vertical lines mark rest-frame wavelength of the SDSS u and r filters.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: The black hole mass and observer-frame e-folding rise and decline timescales of 33 TDEs.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption: Distributions of the angular separation between the location of a simulated neutrino source and the associated hot spot with L > 3.0 for the northern (left) and southern (right) sky. In both panels, the solid and dashed red lines indicate the median and the 90% quantile of the distribution, respectively.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption: Comparison of the sensitivity to an E −2 astrophysical neutrino flux across the sky for the analysis used in this work and the one published in Aartsen et al. (2020).
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  p local for the 5BZCAT−neutrino hot spot spatial correlation as a function of the association radius (r assoc) and for various minimum significance thresholds for the hot spots (﹩{L}_{\min }﹩) for the 7 yr samples. The correlation analysis is performed both in the southern sky (left) and in the northern sky (right). The two panels also show the significance level corresponding to the number of Gaussian-equivalent standard deviations. The left panel shows that we reproduce the results presented in Buson et al. (2022a, 2022b).
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  p local for the RFC−neutrino hot spot spatial correlation as a function of the association radius (r assoc) and for various minimum significance thresholds for the hot spots (﹩{L}_{\min }﹩) for the 7 yr samples. The correlation analysis is performed both in the southern sky (left) and in the northern sky (right). The two panels also show the significance level corresponding to the number of standard deviations.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption: Decl. distribution of the sources in the 5BZCAT (left) and in the RFC (right) in red, compared to the cosine distribution in blue. Note that the expected uniform distribution is not a perfect cosine because the Galactic plane is removed, as done in the source catalogs.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  L sky map of the point-source likelihood search in the Northern and Southern Hemispheres. The map is shown in equatorial coordinates (R.A. on the horizontal axis and decl. on the vertical one) on a Hammer–Aitoff projection. The color scale indicates the L values obtained from the maximum likelihood ratio analysis performed at each pixel in the sky. The dashed red line indicates the horizon, separating the northern and southern skies at −5°.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  p local for the 5BZCAT−neutrino hot spot spatial correlation as a function of the association radius (r assoc) and for various minimum significance thresholds for the hot spots (﹩{L}_{\min }﹩) for the 10 yr neutrino sample. The correlation analysis is performed both in the southern sky (left) and in the northern sky (right). The two panels also show the significance level corresponding to the number of standard deviations.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  p local for the RFC−neutrino hot spot spatial correlation as a function of the association radius (r assoc) and for various minimum significance thresholds for the hot spots (﹩{L}_{\min }﹩) for the 10 yr neutrino sample. The correlation analysis is performed both in the southern sky (left) and in the northern sky (right). The two panels also show the significance level corresponding to the number of standard deviations.
Paper: DKIST Unveils the Serpentine Topology of Quiet Sun Magnetism in the Photosphere
Authors: Ryan J. Campbell, P. H. Keys, M. Mathioudakis, F. Wöger, T. Schad, A. Tritschler, A. G. de Wijn, H. N. Smitha, C. Beck, D. J. Christian, D. B. Jess, R. Erdélyi
Figure caption: Three case studies of small-scale magnetism, including a serpentine-like magnetic configuration (top row), two magnetic loops (middle rows), and a magnetic granule (bottom row). From left to right is Stokes I at 6303.17 Å, L tot, Stokes V at 6302.45 Å, v LOS, γ, ϕ, and α  m  B. The last four parameters are derived from SIR inversions with one magnetic and one nonmagnetic model atmosphere (1C configuration). The scanning direction (i.e., solar X) is shown on the x-axis, and the slit direction (i.e., solar Y) is shown on the y-axis. The labeled (A.1, B.1, B.2, C.1–C.4) markers highlight the spatial locations of the sample pixels; the full Stokes vector from pixel A.1 is shown in Figure 3, B.1 is shown in Figure 5, B.2 is shown in Figure 6, C.1 is shown in Figure 7, C.2 is shown in Figure 8, and the circular polarization profiles for C.3 and C.4 are shown in Figure 9. The region outlined by the cyan box in the top row is shown in Figure 4.
Paper: DKIST Unveils the Serpentine Topology of Quiet Sun Magnetism in the Photosphere
Authors: Ryan J. Campbell, P. H. Keys, M. Mathioudakis, F. Wöger, T. Schad, A. Tritschler, A. G. de Wijn, H. N. Smitha, C. Beck, D. J. Christian, D. B. Jess, R. Erdélyi
Figure caption: Sample observed Stokes vector with the best-fit inverted profiles (left panels) and model-associated atmospheres (right panels) whose spatial location is labeled in the serpentine magnetic element in the top row of Figure 2 (pixel A.1). The horizontal dotted–dashed lines show the noise thresholds (±4σ  n ), while the vertical dotted lines indicate the rest wavelengths of the Fe I doublet. The retrieved atmospheric parameters are shown as a function of optical depth. The ϕ, α  m , and v mac values are 107°, 0.47, and 0.015 km s−1, respectively. This inversion is a 1C configuration.
Paper: DKIST Unveils the Serpentine Topology of Quiet Sun Magnetism in the Photosphere
Authors: Ryan J. Campbell, P. H. Keys, M. Mathioudakis, F. Wöger, T. Schad, A. Tritschler, A. G. de Wijn, H. N. Smitha, C. Beck, D. J. Christian, D. B. Jess, R. Erdélyi
Figure caption: Summed power spectrum of the intensity, computed at a wavelength of 6302.47 Å for each step, summed across step positions with greater than the mean continuum intensity contrast of 6.2%. The dotted blue line shows the summed power spectrum windowed by a Hann filter before computing the FFT. The solid red line shows a median filter applied to the Hann-windowed power spectrum. The dashed red vertical line indicates the frequency that equates to a spatial resolution of 0.″08.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Panels (a)–(o): correlations between TDE photometric properties, λ Edd, and M BH. Symbol colors follow the same convention as in Figure 2 and Figure 9. Hollow markers show objects at z > 0.24, where there is an observational bias toward selecting TDEs in higher-mass galaxies. Panel (a): the dotted line shows the expected ﹩{R}_{\mathrm{bb}}\propto {M}_{\mathrm{BH}}^{2/3}﹩ scaling relation in a fiducial cooling envelop model (Metzger 2022); the dashed (﹩{R}_{\mathrm{bb}}\propto {M}_{\mathrm{BH}}^{0.15}﹩) and solid (﹩{R}_{\mathrm{bb}}\propto {M}_{\mathrm{BH}}^{0.09}﹩) lines show the best-fit power laws using all markers and filled markers, respectively (see Section 6.3). Panel (d): the dotted line shows the expected Eddington ratio of peak fall-back accretion rate ﹩{\lambda }_{\mathrm{Edd}}\propto {M}_{\mathrm{BH}}^{-3/2};﹩ the dashed (﹩{\lambda }_{\mathrm{Edd}}\propto {M}_{\mathrm{BH}}^{-0.52}﹩) and solid (﹩{\lambda }_{\mathrm{Edd}}\propto {M}_{\mathrm{BH}}^{-0.74}﹩) lines show the best-fit power laws using all markers and filled markers, respectively (see Section 6.1.3). Panel (e): the dotted line shows the expected fall-back timescale of ﹩{t}_{1/2}\propto {M}_{\mathrm{BH}}^{1/2};﹩ the dashed (﹩{t}_{1/2}\propto {M}_{\mathrm{BH}}^{0.14}﹩) and solid (﹩{t}_{1/2}\propto {M}_{\mathrm{BH}}^{0.16}﹩) lines show the best-fit power laws using all markers and filled markers, respectively (see Section 6.1.2). Panel (p): p-value of Kendall’s tau test for 15 pairs of parameters. The results using 33 TDEs are shown outside the parenthesis, and the results using 28 TDEs at z < 0.24 are shown in the parenthesis. Significant correlations with p < 0.05 are highlighted in red colors.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Upper: the thin lines are the log M BH PDFs of the 33 TDE host galaxies. The think black line shows the total number of detected TDEs per dex, computed by summing over the individual Gaussians and plotted between the peak of the PDF of the lowest BH mass (105.13 M ⊙) and highest BH mass (108.23 M ⊙). The semitransparent region represents the 1σ uncertainties. Lower: the thin dotted lines are the PDFs (in the upper panel) multiplied by ﹩{{ \mathcal R }}_{i}﹩. The solid black curve shows the total optical TDE rate as a function of M BH. From 105.3 M ⊙ to 107.3 M ⊙, the slope follows a power law of ﹩\phi \propto \mathrm{log}{M}_{\mathrm{BH}}^{-0.25}﹩ (red dotted line). We show predictions of two BHMFs (Shankar et al. 2016; Gallo & Sesana 2019) with and without the event-horizon (EH) suppression factor g(M BH) (see Equation (20)), normalized to match the black curve at M BH = 106.5 M ⊙.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption:  M BH vs. M gal for 19 TDEs with M BH measurements inferred from σ *, labeled by IDs in Table 3. The solid red line is a linear fit to these objects (Equation (5)). The solid, dashed, and dash–dotted blue lines are relations presented in Greene et al. (2020; supplemental Table 5), derived using all galaxies (with upper limits on M BH), late-type galaxies (with upper limits), and early-type galaxies. The thin dotted and long dashed gray lines are from Reines & Volonteri (2015) using AGN and inactive galaxies.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Rest-frame g-band light curves of the 33 TDEs in our sample. The solid lines show the best-fit models.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Upper: redshift vs. log L g for 33 TDEs in this work (circles) and 13 TDEs used by van Velzen (2018; crosses). The boundaries of the 9 luminosity bins used in this work are indicated by the vertical dotted lines. Lower: TDE LF in rest-frame g band. We show the single and double power-law fits as well as the two LFs presented in van Velzen (2018).
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: ESI spectra of 17 TDE host galaxies arranged in order of decreasing σ *. The black lines are the data, and the red lines are the models. Prominent host galaxy absorption lines are indicated by the vertical lines. Masked regions are not plotted. The median S/N of the fitted wavelength range of each spectrum is given in Appendix A (Table 8).
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Upper: redshift vs. log L bb for 33 TDEs in this work (circles), and vs. the peak X-ray luminosity for 13 SRG-selected TDEs presented by Sazonov et al. (2021). Lower: TDE LF in terms of peak UV and optical blackbody luminosity or peak 0.2–6 keV X-ray luminosity. The dotted and solid gray lines show the single power-law (Equation (17)) and double power-law (Equation (18)) fits. The dashed green line shows the X-ray LF given by Sazonov et al. (2021). For the dashed and dotted lines, 1σ uncertainties are indicated with the semitransparent regions.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: ZTF and ATLAS light curves of AT2021yzv, overplotted with the best-fit models in the ZTF r band. Detections at >4σ are shown with high opacity. A power-law function provides a better description for the rise profile.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: TDE rate as a function of R bb.
Paper: Correlating High-energy IceCube Neutrinos with 5BZCAT Blazars and RFC Sources
Authors: Chiara Bellenghi, Paolo Padovani, Elisa Resconi, Paolo Giommi
Figure caption:  p local for the blazar−neutrino hot spot spatial correlation as a function of the association radius (r assoc) and for various minimum significance thresholds for the hot spots (﹩{L}_{\min }﹩) for the 10 yr northern neutrino sky. A hot spot with ﹩{L}_{\min }=3.7﹩ at the location of TXS 0506+056 was added to the hot spot list. The correlation analysis uses the 5BZCAT (left) and RFC (right) catalogs. The two panels also show the significance level corresponding to the number of Gaussian-equivalent standard deviations.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption:  g–r evolution of the 55 TDE candidates. The top panel shows 5 objects without spectroscopic classifications, and the other 8 panels show 50 spectroscopically classified objects. Color has been corrected for Galactic extinction.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: UV and optical properties of AT2020yue. Upper: ZTF and UV light curves of AT2020yue. Detections at >3σ are shown with high opacity; other observations are shown in semitransparent. Middle: optical spectra of AT2020yue. For comparison, we also show the host-subtracted optical spectrum of PS1-11af (Chornock et al. 2014), and the host galaxy model derived in Section 4.2.2. Bottom: the +595 days spectrum zoomed around Hα. To highlight the broad Hα component, the y-axis is shown in linear-scale below 1.2, and in log scale above 1.2.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Optical spectra of 10 objects. Strong atmospheric telluric features have been masked. The top 9 objects show broad emission lines characteristic of spectral classes of TDE-H, TDE-H+He, and TDE-He. In a few objects, we have subtracted the blue blackbody continua and masked strong host galaxy narrow emission lines. The bottom spectrum was obtained for the host galaxy of AT2020abri.