adsabs/AstroCLIMB huggingface dataset:
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: Prime-Cam instrument design showing the placement of the seven instrument module entrance windows including the five polarization-sensitive modules at nominal band center frequencies from 220 to 850 GHz, and the two spectrometer (EoR-Spec) modules. (Vavagiakis et al. 2018).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: H I-to-H2 transition in a plane-parallel slab with CR ionization, as a function of the ratio χ 0/n. The CR ionization rate is attenuated following the prescription given by Equation (55). The top row shows the total hydrogen column N trans at which the transition occurs (﹩2{x}_{{{\rm{H}}}_{2}}=0.5﹩), and the middle bottom rows show the H I column integrated up to the point where N = 1022 and 1023 cm−2, respectively. Each column shows results from a slab with different gas density. The symbols show the numerical results with (filled) and without (open) CR ionization. The symbol color indicates the strength of the unattenuated CR ionization rate ξ cr,0, and shape indicates spatial resolution. We only show cases in which N trans is resolved by more than three cells. The gray dashed lines show the analytic approximations for N trans and N HI,tot by Bialy & Sternberg (2016) in the absence of CR ionization (Equations (60) and (63)). Including CR ionization can significantly increase the shielding required for H2 to form.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: PDR test: a plane-parallel, uniform-density slab of gas in thermal and chemical equilibrium for ﹩{Z}^{{\prime} }=1﹩. The slab is illuminated by a unidirectional FUV radiation field χ 0 with the unattenuated CR ionization rate ξ cr,0 = 2 × 10−16 s−1. From top to bottom, panels show as functions of perpendicular hydrogen column density N (or A  V  = N/[1.87 × 1021 cm−2]; top x-axis) the temperature, chemical abundances, cooling rate per H, heating rate per H, and normalized radiation field and CR ionization rate. The left column shows the case with density n = 102 cm−3 and low FUV intensity (χ 0 = 1), while the middle and right columns show cases with density n = 103, 104 cm−3 and high FUV intensity (χ 0 = 102, 104). The results from full chemistry code calculations (Gong et al. 2017) are shown as dashed lines for comparison (except for dust temperature T  d , which is set to a fixed value T  d  = 10 K in Gong et al. (2017).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Time evolution of various quantities of an expanding H2 region driven by thermal pressure of ionized gas. The top row shows the IF radius on linear (top left) and log (top middle) axes and time step size (top right). The bottom row shows radial momentum (bottom left), ionized gas mass (bottom middle), and the fraction of ionizing photons absorbed by neutral gas (bottom right). Models with ﹩{Z}^{{\prime} }=1﹩ and 0.1 are shown as blue and red lines, respectively. We compare runs adopting different time step size Δt for the hydrodynamics and radiation updates. In model A/B (dotted/dashed lines), Δt is constrained by 10%/100% of the global minimum of the cooling and chemical timescales. In model C (thick solid line), Δt is constrained by the usual CFL condition for MHD. We also show the model in which radiation pressure is turned on (model ﹩{{\rm{A}}}^{{\prime} };﹩ thin solid line). In the top left and top middle panels, the dashed gray lines show the analytic prediction for the expansion of a D-type IF by Hosokawa & Inutsuka (2006). The thin solid gray lines in the top middle panel indicate the initial Strömgren radius accounting for the effect of dust absorption (Petrosian et al. 1972). The dashed gray lines in the bottom left and bottom middle panels show the scaling relation expected from Equations (68) and (66) using the Hosokawa & Inutsuka solution.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: SNR properties when cooling becomes important, defined by the time at which the total energy falls below 70% of the injected energy (the “shell formation” time t sf). From top to bottom, we show age, radial momentum, mass, and radius of the SNRs. In columns from (a) to (c), results are from models using cooling from (a) nonequilibrium hydrogen ionization with a neutral background (NEI-N), (b) nonequilibrium hydrogen ionization with an ionized background (NEI-I), and (c) CIE. The thin lines in (c) show fits to the simulation data (Equations (64a)–(64d)). In column (d), we compare all ﹩{Z}^{{\prime} }=1﹩ models; note that the NEI-I (dotted line) results are nearly identical to CIE (dashed line).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: H I-to-H2 transition in a plane-parallel gas slab without CR ionization. The symbols indicate the transition hydrogen column (N 1,trans) at which ﹩{x}_{{\rm{H}}}=2{x}_{{{\rm{H}}}_{2}}﹩ for various gas densities (n = 10–104 cm−3) and FUV incident radiation fields (χ 0 = 10−1–105). Results for different spatial resolution (Δx = 10−3–1 pc) are indicated with different symbols, and we only show cases in which the transition column is resolved by more than three cells. Our numerical results agree well with the analytic approximation by Bialy & Sternberg (2016) (dotted lines).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as Figure 5, except that we adopt a density-dependent shielding treatment for the FUV intensity and CR ionization rate (see text for details). The equilibrium curves in which H2 rovibrational cooling is turned off are shown as dashed–dotted lines.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Radial profiles of expanding H II regions driven by thermal pressure of ionized gas. The background medium has density n 0 = 102 cm−3, and the metal and dust scaled abundance ﹩{Z}^{{\prime} }=1﹩ (blue) or 0.1 (red). We show radial profiles of density, gas and dust (thin lines) temperature, and abundances of H I and H2 at times t = 0.29, 0.59, 1.47, and 2.93 Myr. The time step size for radiation and hydrodynamics updates is set to 10% of the global minimum of the chemical and cooling timescales (model A).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Time evolution of the shell radius for radiation pressure–driven bubble expansion in a uniform medium (n 0 = 104 cm−3) for ﹩{Z}^{{\prime} }=1﹩ (blue) and 0.1 (red) and for grid spacings Δx = 9.4 × 10−2 pc (thin lines) and 4.7 × 10−2 pc (thick lines). The gray dashed line shows the similarity solution for the thin shell expansion (Equation (70)).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as Figure 6, but for shielded gas (with H2 rovibrational cooling) as shown in Figure 8 with χ 0 = 1 and ξ cr = 2 × 10−16 s−1.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: The discriminator of DCGAN designed in this paper. The input of this discriminator is a pulsar-candidate image of size 48 × 48. The four convolution layers in the middle extract the features of the image. Finally, the probability of the real image is obtained by a sigmoid function.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: The network structure of ResNeXt designed in this paper. The left side of the figure shows the structure of ResNeXt as a whole. The input is a gray-scale pulsar-candidate image, and the output is the predicted probability that the candidate is a positive or negative sample. The middle shows a sequential, which is made up of three BottleneckBlocks and each BottleneckBlock includes 64 groups. The structure of each group is shown in the right.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: The generator of DCGAN designed in this paper. The input to the generator is a random uniformly distributed noise of 100 dimensions. There are four transposed convolution layers in the middle. The final output is a generated pulsar-candidate image.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: Diagnostic plots of a positive sample from the HTRU Medlat data set (Morello et al. 2014). For a real pulsar there are one or more distinct vertical stripes in the FPP and TPP. The profile histogram displays one or more wave peaks. In addition the DM curve has a peak at a nonzero value.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: Real positive sample images that are from real confirmed pulsars. Panels (a)–(f) are all FPP. The horizontal direction is the phase and the vertical direction is the frequency.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: Generated positive sample images. Panels (a)–(f) are all FPP. The horizontal direction is the phase and the vertical direction is the frequency.
Paper: Pulsar-candidate Selection Using a Generative Adversarial Network and ResNeXt
Authors: Qian Yin, Yefan Li, Jiajie Li, Xin Zheng, Ping Guo
Figure caption: Diagnostic plots of a negative sample from the HTRU Medlat data set (Morello et al. 2014). There are no distinct vertical lines in the FPP and TPP and no obvious peaks in profile histogram and the DM curve.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: (Top) Dust extinction (solid) and absorption (dashed) cross sections at UV and optical wavelengths for the Weingartner & Draine (2001b) Milky Way grain size distribution with ratio of visual extinction to reddening R  V  = 3.1 and C abundance parameter b C = 55.8 ppm. (Middle) SED in the UV and optical bands for a coeval population of stars sampling the Kroupa IMF, with ages 1, 2, ⋯, 50 Myr. (Bottom) Various estimates of the local ISRF. The thick blue and red lines show the estimate at the disk midplane using (1) the light-to-mass ratio shown in the middle panel, (2) history of SFR at the solar circle based on Zari et al. (2022), and (3) an attenuation factor that depends on dust optical depth of the gas disk (Ostriker et al. 2010); the thin blue and red lines show the corresponding estimate without the attenuation factor (see text for details). Other lines are the estimate of the local ISRF by Draine (1978) (black solid line), Mathis et al. (1983) (green dashed line), van Dishoeck & Black (1982) (black dotted line), and Habing (1968) (magenta dotted line). For comparison, we also show the UVB model of Faucher-Giguère (2020) at zero redshift, scaled by 103 times (yellow dashed–dotted line). Estimates based on observations are shown as open squares (Henry et al. 1980) and diamonds (Gondhalekar et al. 1980).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Comparison of equilibrium gas properties computed with models originating in the ISM community (Gong et al. 2017; Wolfire et al. 2003; Bialy & Sternberg 2019; Koyama & Inutsuka 2002) and the galaxy formation community (Smith et al. 2017; Hopkins et al. 2018; Ploeckinger & Schaye 2020; Rosen & Bregman 1995). For the former, the FUV radiation field is representative of solar neighborhood conditions; for the latter, heating and ionization by metagalactic UVB (but not by low-energy CRs) are included (see text for details). From left to right, panels show thermal pressure, temperature, and electron abundance. The top row shows results for solar metallicity (﹩{Z}^{{\prime} }=1﹩), and the bottom row for low metallicity (﹩{Z}^{{\prime} }=0.1﹩). In the top left panel, the gray-shaded region indicates the observed range of thermal pressure in the local diffuse CNM inferred from C I fine-structure lines (Jenkins & Tripp 2011). Comparison of the cooling functions and specific heating rates for the same models is shown in Figure 18.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: The heating rate per H nucleon (Γ = nΛ) as a function of density (left) and the cooling function (Λ) as a function of temperature (right) for models shown in Figure 17 with ﹩{Z}^{{\prime} }=1﹩ (top) and 0.1 (bottom).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Colored lines show equilibrium phase diagrams (top) and heating/ionization curves (bottom) in the presence of UVB of Faucher-Giguère (2020) at two redshifts z = 0 (solid lines) and 3 (dashed lines). The equilibrium electron abundance is obtained assuming ionizing UVB with (red) and without (blue) the attenuation prescription of Rahmati et al. (2013). For the latter, we additionally include grain PE heating (Γpe) with χ = 1 and ﹩{Z}_{d}^{{\rm{{\prime} }}}=1﹩. The PE heating efficiency is computed using the Weingartner & Draine (2001a) formula, which depends on the grain charging parameter ∝ χ T 1/2/n e. For comparison, the results of our cooling module for the solar neighborhood condition (without UVB) are shown as black solid lines. All curves shown here assume the same cooling function Λ(T) obtained from our model for the solar neighborhood condition (black curve shown in the upper left panel of Figure 18).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: The top left panel shows the luminosity per unit mass of a coeval stellar population in the UV and optical bands as a function of age, based on Starburst99. The purple and gray lines show the energy output rate per unit mass from stellar winds (L  w /M *) and SNe (﹩{L}_{\mathrm{sn}}/{M}_{* }﹩), respectively. The corresponding cumulative energy output per unit mass is shown in the bottom left panel. The right panels show the instantaneous and cumulative momentum output per unit mass.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: (Top) Absorption, extinction, and radiation pressure cross sections per H nucleon, averaged over the SED of a star cluster (middle panel of Figure 20), as a function of the cluster age. (Middle) Mean energy of photons (solid line) and average energy of photoelectrons for PI of H and H2. (Bottom) Average PI cross sections for H and H2.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The C18O (J = 1–0) observation area is drawn with the black solid lines on the H2 column density map. Our map covers a wide area of 1 × 2 square degrees, which is from OMC-1/2/3/4 to L1641N, V380 Ori, and L1641C.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The spatial distribution of starless and protostellar cores in Orion A. The dashed black lines represent the area of four subregions: OMC-1/2/3, OMC-4/5, L1641N, and L1641C. The solid black square is the ONC region, which is analyzed by Paper I.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The spatial distribution of bound starless cores (red dots) and unbound starless cores (blue dots) overlaid onto the integrated intensity map of the C18O (J = 1–0) emission.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of properties of starless cores (solid green line) and protostellar cores (dashed orange line) in Orion A: (a) diameter, (b) aspect ratio, (c) velocity width in FWHM, (d) mass, (e) number density, and (f) virial ratio. In panel (f) the vertical dotted line represents α vir = 2.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 4 for the L1641C area, which is the area 4 in Figure 3.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The enlarged view of OMC-1/2/3 area corresponds to the area 1 in Figure 3.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: Histograms of properties of bounded starless cores (thick solid blue line), and unbounded starless cores (thick dashed cyan line) in Orion A: (a) diameter, (b) aspect ratio, (c) velocity width in FWHM, (d) mass, (e) number density, and (f) virial ratio.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 4 for the L1641N/V380 Ori area, which is the area 3 in Figure 3.
Paper: CARMA-NRO Orion Survey: Unbiased Survey of Dense Cores and Core Mass Functions in Orion A
Authors: Hideaki Takemura, Fumitaka Nakamura, Héctor G. Arce, Nicola Schneider, Volker Ossenkopf-Okada, Shuo Kong, Shun Ishii, Kazuhito Dobashi, Tomomi Shimoikura, Patricio Sanhueza, Takashi Tsukagoshi, Paolo Padoan, Ralf S. Klessen, Paul. F. Goldsmith, Blakesley Burkhart, Dariusz C. Lis, Álvaro Sánchez-Monge, Yoshito Shimajiri, Ryohei Kawabe
Figure caption: The same figure as Figure 4 for the OMC-4/5 area, which is the area 2 in Figure 3.