adsabs/AstroCLIMB huggingface dataset:
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: TESS transit light curve of GJ 367 b and best-fitting model folded at the orbital period of the planet.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Least-squares deconvolved (LSD) Stokes I, V and null profiles of GJ 367. The polarization profiles are shifted vertically and expanded by a factor of 100 relative to the intensity profile. The vertical dashed lines indicate velocity interval adopted for the longitudinal field measurement.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Coadded HARPS spectrum of AU Mic (black line) in the spectral region encompassing the Li I 6708 Å absorption line. Superimposed with a thick red line is the coadded HARPS spectrum of GJ 367, which has been rotationally broadened to match the v sin i ⋆ = 7.8 km s−1 of AU Mic.
Paper: Self-similar Outflows at the Source of the Fast Solar Wind: A Smoking Gun of Multiscale Impulsive Reconnection?
Authors: Vadim M. Uritsky, Judith T. Karpen, Nour E. Raouafi, Pankaj Kumar, C. Richard DeVore, Craig E. Deforest
Figure caption: Probability histograms of the detected transient flow events over the event: (a) lifetime T; (b) transverse flow size L; (c) upward flow velocity v; (d) relative emission intensity δ I/I 0; (e) transported flow volume V; and (f) kinetic energy K of the flow. Mean (μ), median (m), and standard deviation (σ) values are provided for each parameter. The dashed red lines show the log–log slopes of the T, L, V, and K distributions, supplemented by the evaluated power-law exponent values.
Paper: Self-similar Outflows at the Source of the Fast Solar Wind: A Smoking Gun of Multiscale Impulsive Reconnection?
Authors: Vadim M. Uritsky, Judith T. Karpen, Nour E. Raouafi, Pankaj Kumar, C. Richard DeVore, Craig E. Deforest
Figure caption: (a) The number N  f  of distinct identifiable flow fronts on the detrended surfing map vs. the detection threshold. The optimized threshold (0.818) resulting in the largest number of identified flow events (2353) was used for the subsequent spatiotemporal event detection. ((b), (c)) Example of temporal and spatial detrending of the surfing flow map S RMS(t, x) based on the estimated correlation scales. (d) The processed flow map showing the detected flow events marked with random color. Only the events involving more than 10 spatiotemporal pixels were plotted and used for the statistical survey presented in Figure 5 since smaller events are not informative due to the applied image smoothing.
Paper: Self-similar Outflows at the Source of the Fast Solar Wind: A Smoking Gun of Multiscale Impulsive Reconnection?
Authors: Vadim M. Uritsky, Judith T. Karpen, Nour E. Raouafi, Pankaj Kumar, C. Richard DeVore, Craig E. Deforest
Figure caption: Top: spatiotemporal map of the transient outflow in the studied region constructed using the ST technique. The compact blobs shown in red represent starting times and locations of the quasi-periodic propagating fronts (see text for details). Bottom: temporal and spatial autocorrelation functions of the surfing signals; the provided characteristic scales represent the 50% levels and assume an exponential decay.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: The separation distribution of simulated triples compared to the observed Gaia 200 pc sample. We compare the projected separations (R ⊥) between the inner binary and the tertiary of Gaia triples (red) to the final outer semimajor axes R ⊥ of the simulated triples. The solid blue curve is the result of our outer binary (OB) models, and the dashed light blue curve is the result of the independent binary (IB) models (Section 2.2). We explore the effects of both flyby interactions and mass-loss-induced kicks in changing the separation distributions. The first row shows the raw outcome of simulations, without the inclusion of any perturbative mechanisms. The second row takes into account the effect of flyby interactions in unbinding wide triples (e.g., Michaely & Perets 2020). The bottom row takes into account both flyby interactions and the effect of mass-loss-induced kicks in changing the outer separation (a 2) of triples (following El-Badry & Rix 2018). See Section 4 for a detailed comparison between the observed and theoretical samples. For information on how flybys and kicks were incorporated into our simulated triple systems, we refer the reader to Sections 4.2.1 and 4.2.2. Note the agreement between the Gaia distribution and the simulation results in the bottom row.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: We display the flux–magnitude cutoffs used to gather our sample of observed Gaia binaries. Each point on this Gaia HR diagram represents a point source in the Gaia DR3 100 pc sample. For each source, we use the Gaia magnitude (M  G ) as a function of the difference between the Gaia blue (B  p ) and red (R  p ) bands. Objects that lie to the left of the red line in Figure 3 are considered to be single WDs. Objects above the red curve and below the pink curve are identified as unresolved double WD binaries. The range between the magenta and blue lines is the region of WDMS binaries. For more information about the cutoffs, see Section 2.4.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: Time-evolution of the semimajor axis and periastron of the inner binary in a representative triple system. After the 12.5 Gyr, the system became a double WD inner binary orbited by a low-mass main-sequence companion. The oscillating blue line represents the evolution in the triple code, and the red line (labeled COSMIC) shows the binary evolution in COSMIC. As one of the stars in the inner binary evolved into a Giant at 8.2 Gyr (109.91 yr), the binary became tidally locked because e 1 < 0.01 and a 1 ≤ 4Roche2. We then evolved this binary using COSMIC for 1.9 Gyr, until the star evolved into a WD, creating a WDMS binary that is no longer tidally locked. After updating the tertiary star’s orbital parameters, we then inserted this triple back into the triple-evolution code to finish its evolution until 12.5 Gyr. Initially, this system had m 1 = 1.09 M ⊙, m 2 = 1.12 M ⊙, m 3 = 0.68 M ⊙, a 1 = 6.47 au, a 2 = 177.68 au, e 1 = 0.157, e 2 = 0.512, i tot = 55.5°.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: The outer-orbit separation (a 2, top row) and the inner eccentricity (e 1, bottom row), as a function of the inner semimajor axis (a 1) for all WD triples. The right column depicts the 1IB and 1OB runs, for which m 1 = 1 M ⊙ initially, while the left panel plots the models with Kroupa IMFs (i.e., KIB and KOB runs). We show WDMS binaries in blue and WDWD binaries in magenta. Circles represent binaries from the 1IB and KIB models; diamonds represent binaries from the 1OB and KOB models. Gray squares show the initial conditions (IC). The dashed black in the top panel shows the a 1 = a 2 (1:1) line. In the bottom row, the dashed black line shows a constant angular momentum curve.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: The types and fractions of the different triples (top) and mergers (bottom) produced from the three-body simulations. Top: the outer ring represents the type of the inner binary, and the inner ring specifies the type of the third star. The color corresponding to the type of triples is outlined in the legend, where MS is for main-sequence star, RG is for red giant, and WD is for WD. Bottom: distribution of different stellar types of the inner binary before the merger event. The exploded slices correspond to mergers that included at least one WD.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: Initial inner (“in”) and outer (“out”) semimajor axis distributions of the triples for the 1OB, KOB models (top), and 1IB, KIB models (bottom). We also show the Gaussian curve used for our simulated binaries, which is again chosen from the period distribution of Duquennoy & Mayor (1991). This is to illustrate that the OB models had separation samples from this Gaussian curve; for details, see Section 2.2.
Paper: Dynamical Evolution of White Dwarfs in Triples in the Era of Gaia
Authors: Cheyanne Shariat, Smadar Naoz, Bradley M. S. Hansen, Isabel Angelo, Erez Michaely, Alexander P. Stephan
Figure caption: The cumulative distribution function of angular separations for all matched pairs within 200 pc in the Gaia catalog (solid line) compared to the analytic model (dotted) outlined in Equation (D1).
Paper: A Metallicity Dependence on the Occurrence of Core-collapse Supernovae
Authors: Thallis Pessi, Joseph P. Anderson, Joseph D. Lyman, Jose L. Prieto, Lluís Galbany, Christopher S. Kochanek, Sebastian F. Sánchez, Hanindyo Kuncarayakti
Figure caption: The black line shows the cumulative distribution of SFR sorted by [O/H] for all the H II regions in the galaxies, while the red line shows the cumulative distribution of [O/H] at CCSN sites. The shaded regions show 500 bootstrap resamplings of each distribution (using the errors on the measured parameters) and the solid lines show the median of the realizations. The black and red dashed lines show the median [O/H] of the distributions for the H II regions and CCSNe, respectively.
Paper: Self-similar Outflows at the Source of the Fast Solar Wind: A Smoking Gun of Multiscale Impulsive Reconnection?
Authors: Vadim M. Uritsky, Judith T. Karpen, Nour E. Raouafi, Pankaj Kumar, C. Richard DeVore, Craig E. Deforest
Figure caption: (a) An SDO/AIA 171 Å image in the middle of the studied 6 hr time interval, with the ROI bounded by the red lines. The solid line shows the main ROI used for the statistical survey; the dotted line is an ROI with an extended upper boundary used for the speed measurements based on the ST method. A base-10 logarithmic brightness scale is used to enhance the low-intensity structure above the limb. (b) Plane-spherical coordinate representation of the main ROI on panel (a) after radial trend removal. The highly filamented texture of the outflowing plasma is easily seen. (c) One of 1257 studied time–distance plots representing time evolution of the lower corona along the radial slit marked with a red dashed line on panel (b). The gray scales on panels (b) and (c) are calibrated in linear AIA data number (DN) units. A spatiotemporal direction corresponding to the propagation velocity measured by the surfing analysis is shown with a dashed line. (d) The maximized surfing signal S(t, u = v) fulfilling the velocity resonance condition, before and after temporal detrending (gray and black lines, respectively). (e) The rms value S rms of the surfing signal S(t, u) for the time–distance plot in panel (c), showing a well-defined peak at u = v.
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: Maps of γ (top left) and ϕ (top right) in the serpentine structure shown in the first case study of Figure 2. The γ map is shown at ﹩\mathrm{log}({\tau }_{5000\,{\rm{\mathring{\rm{A}} }}})=-1.0﹩. The direction of ϕ is marked with arrows whose value is given after binning by a 3 × 3 kernel for visual clarity. The azimuth is defined such that a value of zero is aligned along the line from solar east to west, increasing counterclockwise. The variation in γ and ϕ is also shown across slices labeled 1 (bottom left) and 2 (bottom right) whose initial and final locations are indicated by the blue dashed lines. The dotted lines show the variation in γ at optical depths between ﹩\mathrm{log}({\tau }_{5000\,{\rm{\mathring{\rm{A}} }}})=-2.0﹩ and 0.0, while the solid red lines show the variation in ϕ across the slices. The dashed gray horizontal lines mark the 90° polarity inversion point for γ.
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: Two solutions to the Stokes vector belonging to pixel B.1 based on two magnetic models (2C) and one magnetic model (1C). The Stokes V signal has a complex shape. In the left column, the red solid lines show the synthetic Stokes vector for 2C, and the blue dotted lines show the same for 1C. The model parameters for 2C and 1C are shown in the middle and right columns, respectively. The location of this pixel is indicated in Figure 2. For 2C, the α values of models 1 and 2 are 0.93 and 0.07, respectively; the ϕ values are 27° and 191°, respectively; and the v mac is 0.77 km s−1 for both models. For 1C, the α values of models 1 and 2 are 0.17 and 0.83, respectively; the ϕ value is 22°; and the v mac is 0.94 km s−1 for both models.
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: Same as Figure 3 but for vector C.1. The filling factors of models 1 and 2 are 0.79 and 0.21, respectively, while the ϕ value is 146°. The v mac is 0.73 km s−1 for both models. This inversion is a 1C configuration. The Stokes V signal has a single lobe.
Paper: Self-similar Outflows at the Source of the Fast Solar Wind: A Smoking Gun of Multiscale Impulsive Reconnection?
Authors: Vadim M. Uritsky, Judith T. Karpen, Nour E. Raouafi, Pankaj Kumar, C. Richard DeVore, Craig E. Deforest
Figure caption: ST analysis of the coronal outflow speed. (a) Speed dependence of the surfing rms for each location on the limb. Each vertical slice represents a S rms(u) dependence such as that plotted on Figure 1(e), with the blue dots showing the position of the resonance maximum used to identify the propagation speed. (b) Fourier power spectra of the resonance surfing signals for different limb positions. The blue dots show the spectral peaks used to evaluate the dominant frequency. Temporal trends longer than 20 minutes were removed for a more accurate velocity estimation. (c) Resonance value S RMS(u = v) representing the characteristic amplitude of the propagating quasi-periodic disturbance at each location.
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: Same as Figure 5 but for the Stokes vector belonging to pixel B.2. For 2C, the α values of models 1 and 2 are 0.83 and 0.17, respectively; the ϕ values are 158° and 23°, respectively; and the v mac is 0.71 km s−1 for both models. For 1C, the α values of models 1 and 2 are 0.93 and 0.07, respectively; the γ and ϕ values for model 1 are 90° and 203°, respectively; and the v mac is 0.94 km s−1 for both models. There is no significant Stokes V signal.
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: Same as Figure 3 but for vector C.2. The filling factors of models 1 and 2 are 0.31 and 0.69, respectively, while the γ and ϕ values are 78° and 152°. The v mac is 0.95 km s−1 for both models. This inversion is a 1C configuration. The Stokes V signal exhibits a regular double-lobed, antisymmetric shape.
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: The Stokes V profiles from pixels C.3 and C.4 are shown in the left and right panels, respectively. Profile C.3 has the WFA fit obtained from the derivative of Stokes I (blue dashed line) overplotted. Both profiles have the synthetic SIR profile overplotted (red solid line). The horizontal gray dashed–dotted lines show the 4σ  n  threshold, and the vertical blue dotted lines show the locations of the blue and red lobes used for the SFA estimate for B.
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: Panel (a): the dotted thin lines represent the values of ﹩{{ \mathcal R }}_{i}﹩ (Equation (7)) multiplied by the individual PDFs of log M gal. The solid thick curve shows the total optical TDE rate as a function of M gal, plotted between the peak of the PDF of the lowest galaxy mass (109.17 M ⊙) and highest galaxy mass (1011.03 M ⊙). The semitransparent region represents the 1σ uncertainties. Panels (b)–(d): the observed optical TDE galaxy mass functions in three bins of ﹩{ \mathcal C }﹩ (Equation (23)). The dashed–dotted lines show the local GMFs multiplied by ﹩{M}_{\mathrm{gal}}^{-0.41}﹩ and scaled to match the observation at M gal = 1010 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: Host galaxies of the TDE sample on the 0,0 u − r vs. M gal diagram, labeled by the IDs in Table 3. The background contours represent a comparison sample of galaxies from SDSS (see text). The region of green valley defined by Schawinski et al. (2014) is denoted by the light green band. In this work, we define a narrower region of green valley (dark green band) by following the contour of the SDSS comparison sample. The solid green line marks the middle of the new green valley (Equation (22)).
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: Left: distributions of 13 galaxies on the color–mass diagram in both this work and Hammerstein et al. (2023). Data points for the same object are connected with the solid black lines. The dashed green line shows the green valley defined by Equation (22). Right: comparison of host galaxy total stellar mass derived in this work and Ramsden et al. (2022).
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: Power-law index of the local BHMF (﹩{{dn}}_{\mathrm{BH}}/d\mathrm{log}{M}_{\mathrm{BH}}\propto {M}_{\mathrm{BH}}^{p}﹩) from the optical TDE mass function (asterisks) with two assumptions on β (see Equation (20)), X-ray nuclei observations (circle, Gallo & Sesana 2019), GMF+scaling relations (squares, Greene et al. 2020), and SAMs (diamonds, Chadayammuri et al. 2023).