adsabs/AstroCLIMB huggingface dataset:
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: 1″ ×  0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 finding charts of the regions surrounding the positions of M53A in the F275W filter. In this panel, the green cross and circle indicate the pulsar position shown in Table 1 and a radius of 3σ (∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩051), using the optical uncertainty due to the cross-correlation between HST and Gaia DR3.
Paper: Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients
Authors: Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia, Xu Kong
Figure caption: An illustration of the simplified model of two primary modes of galaxy disk formation: Coplanar Inflow Mode (left), where coplanar inflow drives disk evolution, and Discrete Evolution Mode (right), where different parts or radii of galaxies evolve independently. The illustration includes both the edge-on view (top) and face-on view (bottom) of the gas disk, with the disk planes rendered in blue and the gas inflow in green. Arrows indicate the trajectories of gas inflows.
Paper: Thirty-five Years of Timing of M53A with Arecibo and FAST
Authors: Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li, Lei Qian
Figure caption: Timing residuals from the best-fit timing models presented in Table 1 as a function of the observation date for M53A.
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption: Time and ϕ average of the radial force balance as a function of the polar angle for an MAD around a rotating BH with spin a = 0.94 at r = 7rg for simulations with the cooling rate increasing from ﹩\dot{M}=1{0}^{-7}{\dot{M}}_{{\rm{Edd}}}﹩ (top left) to ﹩\dot{M}=1{0}^{-4}{\dot{M}}_{{\rm{Edd}}}﹩ (bottom right). We show the contribution of the gradient of the thermal pressure (green), of the magnetic stresses (blue), and of the inertia (orange). Each component is normalized by gravity. The vertical dashed red lines show the disk thickness at this radius. In all cases, the dynamical component dominates. As cooling increases, the contribution of the thermal pressure decreases, while that of the magnetic stresses increases. However, the contribution of the magnetic stresses saturates for a mass accretion rate around ﹩1{0}^{-5}{\dot{M}}_{{\rm{Edd}}}﹩. At an even larger mass accretion rate, the smaller contribution of the gas (thermal) pressure is replaced by the contribution of inertia.
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption: Time and ϕ average contributions to the radial force balance at the equator as a function of the radius. BH spin a = 0.94 is assumed. Mass accretion rate increases from ﹩\dot{M}=1{0}^{-7}{\dot{M}}_{{\rm{Edd}}}﹩ (top left) to ﹩\dot{M}=1{0}^{-4}{\dot{M}}_{{\rm{Edd}}}﹩ (bottom right). We show the contribution of the thermal pressure gradient (green) and of the magnetic stresses (blue), as well as of the inertia (orange). Each component is normalized by gravity. When the cooling rate increases, the contribution of the thermal pressure decreases, while that of the magnetic stresses increases. However, the contribution of the magnetic stresses saturates for a mass accretion rate around ﹩1{0}^{-6}{\dot{M}}_{{\rm{Edd}}}﹩. At larger mass accretion rates, the smaller contribution of the gas pressure is balanced by the increase in the contribution of inertia.
Paper: Radiative Cooling Changes the Dynamics of Magnetically Arrested Disks
Authors: Akshay Singh, Damien Bégué, Asaf Pe'er
Figure caption:  ﹩{\dot{M}}_{{\rm{crit}}}﹩ is a transition in the disk–jet evolution system for both the MAD parameter and the jet efficiency. The left panels show the time-averaged MAD parameter as a function of target mass accretion rate ﹩\dot{M}﹩ for several spins a ∈ {−0.94, −0.5, 0, 0.5, 0.94}. The simulations without cooling are represented for convenience with a mass accretion rate of ﹩1{0}^{-8}{\dot{M}}_{{\rm{edd}}}﹩. For all spins, the MAD parameter is changing around ﹩1{0}^{-6}{\dot{M}}_{{\rm{edd}}}﹩, in agreement with the findings of Section 2. For positive spins, it is decreasing, while for negative spins, it first increases and then decreases. The right panel shows the time-averaged jet efficiency as a function of the targeted mass accretion rate. As the mass accretion rate increases, namely, as cooling increases, the jet efficiency decreases sharply for large (∼0.9) positive spins, while it is steadily increasing for lower spins.
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: Top panel: final flux-calibrated NIRSpec/PRISM (blue) and MIRI/LRS (red) spectra of SIMP 0136+0933, compared to the spectrum presented in J. M. Vos et al. (2023; black) and error (shaded in gray). For the NIRSpec and MIRI spectra, each spectrum is plotted individually. Notable absorption features are indicated by horizontal black lines and their labels. For each instrument, we plot each spectrum individually, so the observed spread is a result of both noise and intrinsic variability. Bottom panel: minimum spectrum subtracted from the maximum spectrum. The maximum and minimum spectra were identified using the 4.5–5.1 μm light curve (Figure 4).
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: Left: variability map showing the reduced NIRSpec/BOTS spectroscopic relative light curves. The variability map is a 2D representation of the relative flux as a function of time and wavelength. Right: binned light curves for NIRSpec. The data are binned by 0.2 μm in wavelength and 1 minute in time. The gray vertical lines at 1 hr mark the approximate minimum of the light curves and denote the “start” of one full rotation (2.4 hr) of the object. The data used to create the variability map and light curves are available on the SIMPLE archive.
Paper: The JWST Weather Report from the Isolated Exoplanet Analog SIMP 0136+0933: Pressure-dependent Variability Driven by Multiple Mechanisms
Authors: Allison M. McCarthy, Johanna M. Vos, Philip S. Muirhead, Beth A. Biller, Caroline V. Morley, Jacqueline Faherty, Ben Burningham, Emily Calamari, Nicolas B. Cowan, Kelle L. Cruz, Eileen Gonzales, Mary Anne Limbach, Pengyu Liu, Evert Nasedkin, Genaro Suárez, Xianyu Tan, Cian O'Toole, Channon Visscher, Niall Whiteford, Yifan Zhou
Figure caption: Left: variability map showing the reduced MIRI/LRS spectroscopic light curves. The variability map is a 2D representation of the relative flux as a function of time and wavelength. Right: binned light curves for MIRI. The data are binned by 0.5 μm in wavelength and 1 minute in time. The gray vertical lines at 3.4 and 5.8 hr represent one complete rotation (2.4 hr) of the object. The data used to create the variability map and light curves are available on the SIMPLE archive.
Paper: In Situ Formation of Star Clusters at z > 7 via Galactic Disk Fragmentation: Shedding Light on Ultracompact Clusters and Overmassive Black Holes Seen by JWST
Authors: Lucio Mayer, Floor van Donkelaar, Matteo Messa, Pedro R. Capelo, Angela Adamo
Figure caption: Top panel: stellar mass histograms for the identified star clusters in the three galaxies, Halo 0 being the primary galaxy, Halo 1 the most massive galaxy companion, and Halo 47 the lowest-mass galaxy companion. Middle panel: distribution of gas fractions of the star clusters in the three galaxies. Both of these panels are scaled such that the cumulative total of all star clusters equals 1. Bottom panel: time evolution of the mass distribution of stellar clusters in the primary galaxy, starting from the first snapshot from which the group finder first identifies gravitationally bound structures. The histograms in this panel are normalized so that the cumulative mass of star clusters in the final snapshot is set to 1.
Paper: In Situ Formation of Star Clusters at z > 7 via Galactic Disk Fragmentation: Shedding Light on Ultracompact Clusters and Overmassive Black Holes Seen by JWST
Authors: Lucio Mayer, Floor van Donkelaar, Matteo Messa, Pedro R. Capelo, Angela Adamo
Figure caption: Color-coded density maps showing the location of the galaxy in the analyzed volume (top panels), the gas component of the disk, viewed face-on and side-on (left-hand panels), and the stellar distribution, also viewed face-on and side-on (right-hand panels) for, respectively, the primary galaxy (Halo 0), the intermediate-mass galaxy (Halo 1), and the lowest-mass galaxy (Halo 47), whose properties are more akin to those in the Cosmic Gems system. The top panels show the subvolume of radius to be about half the virial radius, well within the region in which particle splitting was applied (see L. Mayer et al. 2024). The rectangles in the side-on views represent the region of the disk where the stellar, gas, and dark matter masses (Ms, Mg, and Md, respectively) were calculated, with values presented in the rightmost panel in solar masses. The density maps depict the simulation approximately 5.6 Myr after the galaxy merger, near the end of the simulation analyzed in this work.
Paper: In Situ Formation of Star Clusters at z > 7 via Galactic Disk Fragmentation: Shedding Light on Ultracompact Clusters and Overmassive Black Holes Seen by JWST
Authors: Lucio Mayer, Floor van Donkelaar, Matteo Messa, Pedro R. Capelo, Angela Adamo
Figure caption: Radial distribution (top panel) of the stellar clusters in Halo 0 and mean age distribution (bottom panel) of clusters identified in all three galaxies at the end of the simulation. For the radial distribution, we show the evolution of star clusters only in the massive galaxy, Halo 0, as it provides a much larger statistical sample. The repeated occurrence of peaks of the distribution in certain locations is related to dense ringlike overdensities in which fragmentation occurs repeatedly. The timescales probed are not long enough to witness the expected smearing of such features by migration. The normalization of the histograms is the same as in Figure 2.
Paper: In Situ Formation of Star Clusters at z > 7 via Galactic Disk Fragmentation: Shedding Light on Ultracompact Clusters and Overmassive Black Holes Seen by JWST
Authors: Lucio Mayer, Floor van Donkelaar, Matteo Messa, Pedro R. Capelo, Angela Adamo
Figure caption: Correlation between stellar surface density, ﹩{{\rm{\Sigma }}}_{{M}_{\star }}﹩, and half-mass radius of clusters, stacking results for all three galaxies at the final time and including also the results at different times for the primary galaxy. Gray dashed lines represent star clusters of similar mass, whereas the green line shows the stellar density–radius relation for clusters in local galaxies, following the best fit model from G. Brown & O. Y. Gnedin (2021) using clusters from the LEGUS survey. The purple arrows represent the stellar surface density and radius of clusters identified in the Cosmic Gems galaxy (A. Adamo et al. 2024). The quoted radius refers to the half-light radius, which provides a lower bound for the cluster’s size compared to the half-mass radius. The purple shaded region indicates where the clusters would lie depending on their radius.
Paper: In Situ Formation of Star Clusters at z > 7 via Galactic Disk Fragmentation: Shedding Light on Ultracompact Clusters and Overmassive Black Holes Seen by JWST
Authors: Lucio Mayer, Floor van Donkelaar, Matteo Messa, Pedro R. Capelo, Angela Adamo
Figure caption: Violin plots depicting the distribution of ﹩{{\rm{\Sigma }}}_{{M}_{\star }}﹩ across different redshift intervals of stellar clusters with a Reff below 25 pc. The numbers below the plot represent the number of clusters, with the number of galaxies indicated in parentheses. The blue violins correspond to observed data sets using JWST adapted from E. Vanzella et al. (2022a, 2022b, 2023), A. Claeyssens et al. (2023, 2025), A. Adamo et al. (2024), S. Fujimoto et al. (2024), M. Messa et al. (2025), L. Mowla et al. (2024), and M. Messa et al. (2025, in preparation). In contrast, the red violin corresponds to the data set from this study, where the surface density is computed at the half-mass radius as typically done in the observations.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Corner plot for molecular abundances in the pRT retrievals. Abundances shown are volume mixing ratios. We show the posteriors for our basic model (gray, including H2O, CH4, NH3, CO, CO2) as well as with HCN added (brown), with C2H2 added (pink), and with both HCN and C2H2 added (green). HCN and C2H2 have some overlapping features around 14 μm and have similar impacts on the continuum (see Figure 3; this causes the abundances to be correlated and the inclusion of one species alters the retrieved abundance of the other. For the models without HCN, a spurious tentative detection of CO2 is present in the posteriors, as discussed in the text; this disappears when HCN is included in the models. The retrieved abundances of H2O, CH4, and NH3, all of which have strong features in the MRS spectrum, are largely unchanged by the addition of HCN and C2H2.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Background systematics in the MIRI/MRS data. The central image shows the channel 2A IFU cube (*s3d.fits) collapsed along the wavelength direction, with the source location and the two negative copies of the source (due to the dither strategy of these observations) masked. Even after dither subtraction, the background of these frames is significantly divergent from 0 and varies with wavelength. In the right-hand and lower panels, black lines and gray shading indicate the mean and 1σ variation of the pixel value along each row/column; orange, green, and purple traces indicate the mean and 1σ values for each 1/3 of the wavelength range of the data. These traces show strong variation in the “normalized” background through the cube, which introduces systematics into the spectrum, especially for faint targets such as WISE-0458.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Spectrum of the target before (light colors) and after (dark colors) the residual background correction (Appendix C). We show the full spectrum in the upper panel and zooms of channels 1B and 2A in the middle and lower panels. The correction significantly impacts the overall shape of the spectrum, as well as altering the shapes of some features in the spectrum. In both cases the spectrum is extracted using an aperture radius of 2× FWHM to ensure that the flux of both components of the brown dwarf binary is captured. Each different color represents a different subchannel of the MIRI MRS.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Relative opacities for 14NH3 and 15NH3 at three nominal temperatures, assuming an abundance ratio of 250:1 (similar to the ISM ratio for 14N/15N, A. M. Ritchey et al. 2015), and the ratio between the two opacities in each case. A simplified assumption is that 15NH3 is detectable if it has any features with local opacity stronger than the 14NH3 opacity, i.e., in the green region of the lower panel for each temperature. 15NH3 is only detectable in the coldest brown dwarfs.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Same as Figures 1(b)–(g), but for the spectrum without the background correction applied (see Appendix C for details). The dispersion of data points around the model is larger than in Figure 1, and wavelength-dependent systematics can clearly be seen in the residuals (lower panel), which show structured deviations from 0. Systematics impact the shape and presence of absorption features; retrieved abundances are correspondingly biased.
Paper: HCN and C2H2 in the Atmosphere of a T8.5+T9 Brown Dwarf Binary
Authors: Elisabeth C. Matthews, Paul Mollière, Helena Kühnle, Polychronis Patapis, Niall Whiteford, Matthias Samland, Pierre-Olivier Lagage, Rens Waters, Shang-Min Tsai, Kevin Zahnle, Manuel Guedel, Thomas Henning, Bart Vandenbussche, Olivier Absil, Ioannis Argyriou, David Barrado, Alain Coulais, Adrian M. Glauser, Goran Olofsson, John P. Pye, Daniel Rouan, Pierre Royer, Ewine F. van Dishoeck, T. P. Ray, Göran Östlin
Figure caption: Retrieved pressure–temperature profile of the two brown dwarfs (blue), with the 1σ, 2σ, and 3σ intervals shaded, and the contribution function (gray). The P–T profile is broadly consistent with a self-consistent profile (here an ATMO model (brown) with 550 K, ﹩\mathrm{log}\,g﹩ = 5.5, and chemical equilibrium (M. W. Phillips et al. 2020) for reference). The retrieved profile has slightly less curvature, which is unsurprising, given that we use a regularization term for the P–T profile (see text).
Paper: Isolated Black Holes as Potential PeVatrons and Ultrahigh-energy Gamma-Ray Sources
Authors: Shigeo S. Kimura, Kengo Tomida, Masato I. N. Kobayashi, Koki Kin, Bing Zhang
Figure caption: Gamma-ray spectra from molecular clouds that host IBHs. Top and bottom panels are for a typical case in a typical molecular cloud and for an optimistic case that matches a LHAASO dark source (J0007+5659u), respectively. Their parameter sets are tabulated in Table 1. The thin gray dashed lines represent the LHAASO sensitivity (X. Bai et al. 2019). The black solid and blue dashed curves are our prediction on gamma rays and neutrinos, respectively. The red line with a pink band and the thin dotted line in the lower panel are the observed spectra and upper limit given in the first LHAASO catalog, respectively.
Paper: Isolated Black Holes as Potential PeVatrons and Ultrahigh-energy Gamma-Ray Sources
Authors: Shigeo S. Kimura, Kengo Tomida, Masato I. N. Kobayashi, Koki Kin, Bing Zhang
Figure caption: A schematic picture of our scenario. An IBH in a molecular cloud accretes the surrounding gas, forming an MAD. Protons are accelerated in the MAD, and high-energy protons can escape from the MAD. Some of these protons interact with the ambient gas, emitting TeV–PeV gamma rays that can explain LHAASO dark sources. The majority of the protons escape from the molecular cloud, contributing to the PeV CRs observed on Earth.
Paper: Isolated Black Holes as Potential PeVatrons and Ultrahigh-energy Gamma-Ray Sources
Authors: Shigeo S. Kimura, Kengo Tomida, Masato I. N. Kobayashi, Koki Kin, Bing Zhang
Figure caption: Various timescales as a function of proton energies for a typical IBH in a typical molecular cloud (top) and for parameters that can explain an LHAASO dark source, J0007+05659u (bottom). The solid blue, solid red, and solid black lines represent the cooling, escape, and acceleration timescales, respectively. The thin red dashed and thin red dotted lines represent diffusion and infall timescales, respectively. The thin blue solid, thin blue dashed, and thin blue dotted lines represent pp, pγ, and Bethe–Heitler cooling timescales, respectively. The parameters for both models are given in Table 1.
Paper: Isolated Black Holes as Potential PeVatrons and Ultrahigh-energy Gamma-Ray Sources
Authors: Shigeo S. Kimura, Kengo Tomida, Masato I. N. Kobayashi, Koki Kin, Bing Zhang
Figure caption: Comparison of our model prediction to the observed CR intensity on Earth. The red line represents our prediction. The data points are from KASCADE (W. D. Apel et al. 2013), IceTop (M. G. Aartsen et al. 2019), TALE (R. U. Abbasi et al. 2018), Tibet-III (M. Amenomori et al. 2008), and LHAASO (Z. Cao et al. 2024).
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: The left panel shows the cumulative flux distribution of Class II and embedded sources. The errors (shaded regions) correspond to the uncertainties in the Gaussian fits reported in Table 2. The flux distributions are indistinguishable from each other (see results of K-S test in Table 3). The right panel shows the cumulative distribution of disk inclinations for embedded sources (calculated from the ratios of semimajor to semiminor axes) compared to the isotropic distribution (constructed from 1000 values with uniform distribution in inverse-cosine). The observed distribution of inclinations is also indistinguishable from a random distribution (see K-S test results in Table 3), suggesting that embedded sources are not significantly biased toward highly inclined disks. The inclinations are not expected to follow a Gaussian distribution and hence no Gaussian fit has been included.