adsabs/AstroCLIMB huggingface dataset:
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Least-squares deconvolution profiles of LTT 1445B (green dashed line) and C (blue dashed line) from HARPS data (gray lines), which indicate the rotational broadening for each of the B and C components. The solid red line shows the joint fit of the broadened spectra.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Transit midtimes of the LTT 1445A planets. We show the measured transit midtimes for LTT 1445Ac (orange points, top panel) and for LTT 1445Ab (purple points, bottom panel). The transit midtimes for LTT 1445Ab from TESS, LCO, and MEarth data are noted as filled points, squares, and a star, respectively; transit midtimes for LTT 1445Ac are from TESS data only. As illustrated, the transit times for each planet are consistent with zero (dotted lines), when considering the uncertainties.
Paper: A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
Authors: Jennifer G. Winters, Ryan Cloutier, Amber A. Medina, Jonathan M. Irwin, David Charbonneau, Nicola Astudillo-Defru, Xavier Bonfils, Andrew W. Howard, Howard Isaacson, Jacob L. Bean, Andreas Seifahrt, Johanna K. Teske, Jason D. Eastman, Joseph D. Twicken, Karen A. Collins, Eric L. N. Jensen, Samuel N. Quinn, Matthew J. Payne, Martti H. Kristiansen, Alton Spencer, Andrew Vanderburg, Mathias Zechmeister, Lauren M. Weiss, Sharon Xuesong Wang, Gavin Wang, Stéphane Udry, Ivan A. Terentev, Julian Stürmer, Gudmundur Stefánsson, Avi Shporer, Stephen Shectman, Ramotholo Sefako, Hans Martin Schwengeler, Richard P. Schwarz, Nicholas Scarsdale, Ryan A. Rubenzahl, Arpita Roy, Lee J. Rosenthal, Paul Robertson, Erik A. Petigura, Francesco Pepe, Mark Omohundro, Joseph M. Akana Murphy, Felipe Murgas, Teo Močnik, Benjamin T. Montet, Ronald Mennickent, Andrew W. Mayo, Bob Massey, Jack Lubin, Christophe Lovis, Pablo Lewin, David Kasper, Stephen R. Kane, Jon M. Jenkins, Daniel Huber, Keith Horne, Michelle L. Hill, Paula Gorrini, Steven Giacalone, Benjamin Fulton, Thierry Forveille, Pedro Figueira, Tara Fetherolf, Courtney Dressing, Rodrigo F. Díaz, Xavier Delfosse, Paul A. Dalba, Fei Dai, C. C. Cortés, Ian J. M. Crossfield, Jeffrey D. Crane, Dennis M. Conti, Kevin I. Collins, Ashley Chontos, R. Paul Butler, Peyton Brown, Madison Brady, Aida Behmard, Corey Beard, Natalie M. Batalha, and Jose-Manuel Almenara
Figure caption: Masses and radii for small planets transiting M dwarfs and with precisely (≥3σ) measured masses. The solid curves are illustrative interior structure models of 100% water, 100% magnesium silicate rock, 33% iron plus 67% rock (i.e., Earth-like), and 100% iron from Zeng & Sasselov (2013). LTT 1445Ab and c are depicted by square markers. LTT 1445Ab falls exactly on the composition curve corresponding to the Earth’s ratio of iron (and nickel) to a magnesium silicate. Although we measure the mass of LTT 1445Ac, we have deduced only a lower limit on its radius (green arrow), corresponding to the configuration where the transits are not grazing. If indeed they are not grazing, then the radius of LTT 1445Ac would be the minimum value depicted by the square marker here and would lie on the same composition curve as LTT 1445Ab.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Layout and orientation of the 36 DEIMOS slitmasks across the disk of M33 for the TREX Survey. Each rectangle on the image represents the rough shape and size of a DEIMOS slitmask (approximately 16′by 4′). The cyan bricks were observed in 2016, the green in 2018 and 2019, and the red in 2020. Because of the high density of stars in the central regions, we targeted different stars at the same slitmask position in 2018 and 2019. The 2019 slitmasks placements are the top two green slitmasks. The ellipse represents the approximate location of a break in the exponential surface density profile of the disk at ∼36′ (Ferguson et al. 2007; Barker et al. 2011). The background image of M33 is from the Digital Sky Survey (DSS). In this orientation, north is up, and east is to the left.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Color–magnitude diagrams of the subsets of photometric catalogs used for target selection with the final stellar sample overplotted. The left panel shows stars with HST photometry with the F457W and F814W bands. Most of these stars are from the PHATTER survey, but some are from archival HST images. The center panel shows stars selected from archival HST photometry with the F606W and F814W bands only. The right CMD shows stars selected from the CFHT/Megacam + MegaPipe and from the PAndAS catalog. In each panel, the blue points represent the young stars, the orange represents the intermediate-age stars, and the red squares represent the old stars, and the gray represents a Hess diagram version of the full photometric catalogs. The points outlined in black are young weak CN stars (blue) and intermediate-age carbon stars (orange) with ages derived from spectroscopic analysis instead of CMD divisions; see Appendix for more details. We list the adopted average age for each bin in the legend. All magnitudes have been extinction-corrected.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Map of the intermediate-age and old stars, color-coded by probability of belonging to a dynamically cold component. The ellipse represents the approximate location of the disk break. The center of M33 is marked with a blue cross.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Line-of-sight velocity and velocity dispersion as a function of position for the three broad age bins. The top row shows the young stars. The middle represents the intermediate-age population, and the bottom row shows the old population. For all rows, the color in the first column represents individual line-of-sight velocity. For the second column, color represents the smoothed line-of-sight velocity. The third column shows the local velocity dispersion. The last column shows the size of the radius of the smoothing circle used at that point. The smallest and largest smoothing circle used are also shown. The ellipse represents the approximate location of the disk break. The center of M33 is marked with a black cross. The inner disk (r < 3.75 kpc) has higher velocity dispersion for all age bins, and the young stars show an extended area of high dispersion.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Velocity dispersion distributions for the three age bins. The left panel shows the distributions for the full final population. The right panel shows each age bin divided into an inner (r < 5 kpc) subgroup and an outer subgroup (r > 5 kpc). For all box plots, the shaded box represents the interquartile range, the horizontal line across the box represents the median, and the open circles show the outliers. The outliers are stars with a velocity dispersion that are at least 1.5σ from the first or third quartile value, which is the distance marked by the whiskers. Velocity dispersion does not vary significantly with stellar age, and is on average higher in the inner region.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Velocity dispersion as a function of deprojected radius for the young, intermediate-age, and old populations. Median lines are also plotted. For the intermediate-age and old bins, velocity dispersion is higher in the inner regions than in the outer regions. The old stars show one concentrated area of extreme velocity dispersion, while the young stars show an extended area of high dispersion, and the intermediate-age stars show no high-velocity dispersion. The area of extreme velocity dispersion for the old stars is overlapped with an area that also has extreme velocities for the young stars.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Velocity dispersion as a function of position for the young stars. Panel (a) shows the young stars overplotted on an image of M33 from the DSS. The colors of the points correspond to velocity dispersion. The smaller red points mark H II regions (Hodge et al. 1999). Panel (b) shows a UV image of M33 from the Swift Observatory (image credit: NASA/Swift/Stefan Immle), with a yellow ellipse showing the approximate location of the high-velocity dispersion. (The DSS map is slightly enlarged compared to the image of M33 on the right.) These locations do not have higher concentrations of UV emission than other parts of the disk.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Rotation velocity as a function of deprojected radius. Rotation velocities are calculated with the tilted ring model in Kam et al. (2017; Equation (3)). The top panel shows the youngest bin (light blue), the middle panel shows the intermediate-age group (orange), and the bottom panel shows the old group (red). Each star has been paired with a H I velocity measurement along the same line-of-sight, and the gas is represented by the gray dots. The size of the points is proportional to the ﹩\cos (\theta )﹩ factor in Equation (3), to illustrate the limitations of the equation around the minor axis. The solid (dotted) line shows the median rotation velocity for 0.5 kpc bins for the stars (H I). The deprojection effects around the minor axis cannot explain the full amount of scatter, especially for the gas.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Rotation velocity as a function of deprojected radius for the inner 4 kpc of the disk. Rotation velocities are calculated with the tilted ring model in Kam et al. (2017; Equation (3)). The top row shows the youngest bin (light blue), the middle row shows the intermediate-age group (orange), and the bottom row shows the old group (red). Each star has been paired with a H I (first column), CO (second column), and Hα (third column) velocity measurement along the same line of sight, and the gas is represented by the gray dots. The size of the points is proportional to the ﹩\cos (\theta )﹩ factor in Equation (3), to illustrate the limitations of the equation around the minor axis. The solid (dotted) line shows the median rotation velocity for 0.5 kpc bins for the stars (gas). The deprojection effects around the minor axis cannot explain the full amount of scatter, especially for the gas. The bar is believed to extend to 0.5 kpc (Williams et al. 2021; A. Smercina et al. 2022, in preparation; M. Lazzarini et al. 2022, in preparation).
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Asymmetric drift distributions for the young stars (blue solid), intermediate-age (orange hatched), and old stars (red outline). AD is calculated with respect to the H I using va = vrot,gas − vrot,⋆. The medians are marked by the vertical lines that run from the peak of the corresponding distribution to the top of the plot. There is no clear trend between AD and stellar age, except that the width of the distribution decreases with stellar age.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: AD distributions for the young stars (blue solid), intermediate-age (orange hatched), and old groups (red outline) for the inner 4 kpc. AD is calculated with respect to the H I (left panel), CO (middle panel), and Hα (right panel) using va = vrot,gas − vrot,⋆. The medians are marked by the vertical lines that run from the peak of the corresponding distribution to the top of the plot. On average, the young and old stars have similar median AD values, suggesting there is no trend between AD and stellar age. For the Hα, the gas is lagging the intermediate-age and old stars, resulting in a negative AD, but both AD values are consistent with zero within 1σ.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Cumulative stellar rotation curves for the 216 M33-like analogs from the IllustrisTNG50-1 simulation and the observations presented in this analysis. Left panel: The gray line represents the gas cells, the blue dashed line represent star particles with ages <1 Gyr, the purple line represents star particles with ages 1–5 Gyr, the green line represents star particles with ages 5–10 Gyr, and the red dotted line represents star particles with ages >10 Gyr. The vertical bars represent the width of the distribution (16th–84th percentile) of rotation velocities in a given radial bin. The median rotation velocities of the 0.1 kpc radial bins are shown. Right panel: The magenta filled region represents stellar particles with ages 1–5 Gyr. The width of the filled regions represent the width of the distribution (16th–84th percentile) of rotation velocities in a given radial bin. The observed M33 rotation curves for the three age bins are plotted on top. The observations are consistent with stellar particles ages 1–5 Gyr, which are a similar age to the observed sample.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: Cumulative median AD measurements for M33-like analogs and for observations of young, intermediate-age, and old stars in the disk of M33. The shaded gray regions represent the median AD and the widths of the distribution (16th–84th percentile) of the AD for the analogs. The color points represent the median AD for the young (blue), intermediate-age (orange), and old (red) stars. The black points represent the analog with AD values closest to what is observed. Compared to the whole sample of analogs, the AD from observations is significantly higher for the youngest stars, than that is seen in the simulated analogs.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: A comparison of velocity dispersion as a function of stellar age for the MW (Nordström et al. 2004, black triangles), M31 (Dorman et al. 2015, black squares), M33 star clusters (Beasley et al. 2015, open circles; data later used by Leaman et al. 2017), and M33 (this work, stars). The open stars show the velocity dispersion for intermediate-age and old stars in M33 if halo candidates are not removed. For M31 and M33, the velocity dispersion is in the line of sight, whereas for the MW, the azimuthal component of velocity dispersion is shown. The MW measurements are also in the solar neighborhood, while the measurements of M31 come from across the northern disk, and those from M33 come from across the entire disk. The MW and M31 show a clear increase in velocity dispersion with stellar age. M33 star clusters also show this increase, but the data from this work do not. Additionally, the magnitude of velocity dispersion from this work is much lower than that seen in the M33 star clusters.
Paper: The Triangulum Extended (TREX) Survey: The Stellar Disk Dynamics of M33 as a Function of Stellar Age
Authors: Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, Laurent Chemin, Julianne J. Dalcanton, Benjamin F. Williams, Anil Seth, Ekta Patel, Justin T. Fung, Pujita Tangirala, and Ibrahim Yusufali
Figure caption: A spatial map showing the location of identified weak CN and carbon stars. The color represents the line-of-sight velocity. The weak CN stars have circular symbols and a grayscale bar, and the carbon stars have square symbols and a color bar.
Paper: The Debiased Compositional Distribution of MITHNEOS: Global Match between the Near-Earth and Main-belt Asteroid Populations, and Excess of D-type Near-Earth Objects
Authors: Michaël Marsset, Francesca E. DeMeo, Brian Burt, David Polishook, Richard P. Binzel, Mikael Granvik, Pierre Vernazza, Benoit Carry, Schelte J. Bus, Stephen M. Slivan, Cristina A. Thomas, Nicholas A. Moskovitz, and Andrew S. Rivkin
Figure caption: Histogram of absolute (H) magnitude and diameter of the MITHNEOS data set of 976 NEOs (nbin = 100). H magnitude values were converted to diameters using the measured average albedo pv = 0.22 of the data set. Note the small-size (large-H) end tail of the distribution: this reflects the effort made to observe as many small NEOs as possible in the frame of the survey.
Paper: The Debiased Compositional Distribution of MITHNEOS: Global Match between the Near-Earth and Main-belt Asteroid Populations, and Excess of D-type Near-Earth Objects
Authors: Michaël Marsset, Francesca E. DeMeo, Brian Burt, David Polishook, Richard P. Binzel, Mikael Granvik, Pierre Vernazza, Benoit Carry, Schelte J. Bus, Stephen M. Slivan, Cristina A. Thomas, Nicholas A. Moskovitz, and Andrew S. Rivkin
Figure caption: Number of MBAs selected by DeMeo & Carry (2013) from the SDSS moving object catalog, plotted as a function of asteroid diameter (bin size of 0.5 km) and region of the belt (left: inner belt; middle: middle belt; right: outer belt). The completeness limit of three regions is determined by fitting a power-law function to the size distribution and measuring the size at which the distribution diverges from the power law. The fitting power-law functions to the full population and to the subset of dark spectral classes are represented by the dashed green and black lines, respectively. The fitting function to the subset of bright classes is not shown for better readability. Deriving size completeness limits using the full, compositionally mixed population or using the bright subset leads to an artificially biased distribution against dark objects (Section 3.4). Therefore, we only use the dark subset and derive size completeness limits of 4.0 km for the inner belt, 4.5 km for the middle belt, and 7.0 km for the outer belt.