adsabs/AstroCLIMB huggingface dataset:
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Comparison between the average N2D+ (3–2) and o‐H2D+(11,0–11,1) lines in each core (labeled at the top-left corner of each panel). The N2D+ data are shown with the red histograms, while the o‐H2D+ ones are shown with the black curves. Note that the o‐H2D+ data have been smoothed to the same beam size of the N2D+ cube before extracting the average spectra, which thus are not identical to the ones presented in Figure 5.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Left panel: comparison of the centroid velocities obtained with MCWEEDS on the N2D+ and o‐H2D+ average spectra in the cores where both species have been detected above the 3σ level. The black dashed line shows the 1:1 relation. Right panel: same as in the left panel but for the line widths.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: The color scale shows the continuum emission in Band 7. The white contours represent the o‐H2D+ cores, while the black ones show the cores identified in continuum, which are labeled based on increasing decl.. The beam size and scale bar are shown in the bottom left and right corners, respectively. Cores associated with outflow emission according to Li et al. (2020) are shown with stars.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: The color scale shows the integrated intensity of the o‐H2D+(11,0–11,1) transition as in Figure 1. The black contours shows the N2D+ (3–2) integrated intensity (computed as for o‐H2D+; see Section 2). The levels are: [7,11,15,19]σ, where 1σ = 100 mK km s−1.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Same as Figure 13 but for the column densities. For the four cores where N2D+ is not detected, we show upper limits (in black).
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Maps of best-fit parameters obtained with MCWEEDS. The columns are FWHM, N col, and V lsr, from left to right. The core label is indicated at the top of each central panel. The contours show the continuum emission at levels from 2 to 11σ, in steps of 3σ.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Continuation of Figure B1.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Absolute magnitudes variation with kinematic distance (D) for the newly identified candidate star-forming regions in Paper I. The gray dotted curves show the average detection limit for the minimum integration for eight frames (16.5, 15.5, 11.2, and 7.9 mag for 3.4, 4.6, 12, and 22 μm, respectively; Wright et al. 2010). Right: Absolute magnitudes variation with galactocentric radius (R G) for the newly identified candidate star-forming regions in Paper I. Red circles and yellow squares show candidates whose parental clouds have respective contamination rates of <30% (reliable) and ≥30% (less reliable). The sizes of these markers indicate the respective masses of their parental molecular clouds (small: M CO <103 M ⊙, medium: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). The black dotted lines show the detection limit at D = 16.4 kpc magnitude threshold for comparing the cloud and star formation properties at various distances up to R G = 20.0 kpc (M3.4μm: 0.43 mag, M 4.6μm: −0.57 mag, M 12μm: −4.87 mag, M 22μm: −8.17 mag). Cyan and blue lines show the absolute magnitudes for the A0 and B0 stars in the main sequence (Cox 2000). Note that we used intrinsic V − L colors (V band: 0.5555  μm; L band: 3.547 μm) and the absolute V-band magnitudes of A0 and B0 stars for calculating the apparent magnitudes of those stars for any of the four bands, since infrared colors, such as [3.4]−[22], are negligible for those early-type stars. The blue dotted line shows the 22 μm absolute magnitude for the H II regions ionized by B0 stars (Anderson et al. 2014). Note that 11 star-forming regions with kinematic distances of more than 20 kpc (R G  > 27 kpc) are known to be actually located at a distance of 12 kpc (R G = 19 kpc) based on high-resolution optical spectra (e.g., Smartt et al. 1996; Kobayashi et al. 2008). The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Cloud mass (and CO luminosity) variation with kinematic distance (D) for all BKP clouds (466 clouds) in the outer Galaxy (R G  ≥ 13.5 kpc). The gray dotted curve shows the minimum mass derived from the nominal completeness limit (2.64 K km s−1) of the BKP catalog. Right: Cloud mass (luminosity) variation with galactocentric radius (R G) for all BKP clouds (466 clouds) in the outer Galaxy (R G  ≥ 13.5 kpc). The black dotted lines in the left and right panels show the minimum mass at D = 16.4 kpc and mass threshold (183.6 M ⊙) for comparing the cloud properties at various distances up to R G = 20.0 kpc. The gray areas indicate the concentrated areas considered to be spiral arms. Note that the two molecular clouds with kinematic distances of more than 20 kpc (R G  > 27 kpc) are known to be actually located at a distance of 12 kpc (R G = 19 kpc) based on high-resolution optical spectra (e.g., Smartt et al. 1996; Kobayashi et al. 2008).
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Top left: Normalized number distribution of cloud mass for all 466 BKP clouds in the outer Galaxy. Top right: Normalized number distributions of cloud mass for clouds without candidates (black), clouds with all associated candidates (magenta), and clouds with only reliable associated candidates (red). Bottom left: Cloud mass distribution of all 466 BKP clouds in the outer Galaxy. The black line shows the result of the least-squares fitting with errors for a cloud mass of more than 183.6 M ⊙: log10                       ﹩{dN}/{{dM}}_{\mathrm{CO}}﹩ = −1.36(±0.08)× log10 M CO + 2.89(±0.23). The vertical gray dashed line indicates the mass threshold (183.6 M ⊙). The binning is in logscale, with 25 intervals covering the mass range 100–104.8 M ⊙. Bottom right: Cloud mass distribution of clouds with and without candidate star-forming regions. Magenta squares and black open circles show clouds with and without candidates, respectively. Red circles show only clouds with reliable candidates. The magenta, red, and black dotted lines show the respective results of the least-squares fittings with errors for cloud masses of more than 183.6 M ⊙: log10                       ﹩{dN}/{{dM}}_{\mathrm{CO}}﹩ = −1.04(±0.13)× log10 M CO + 1.43(±0.42) (magenta: all clouds with candidates), log10                       ﹩{dN}/{{dM}}_{\mathrm{CO}}﹩ = −0.99(±0.13)× log10 M CO + 1.33(±0.42) (red: only clouds with reliable candidates), and log10                       ﹩{dN}/{{dM}}_{\mathrm{CO}}﹩ = −1.57(±0.08)× log10 M CO + 3.29(±0.22) (black: clouds without candidates). The error bars show Poisson counting uncertainties.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Cumulative cloud mass distribution of all 466 BKP clouds in the outer Galaxy. Right: Cumulative cloud mass distribution of clouds with and without candidate star-forming regions. Magenta squares and black open circles show clouds with and without candidates, respectively. Red circles show only clouds with reliable candidates. The error bars show Poisson counting uncertainties. The vertical gray dashed line indicates the mass threshold (183.6 M ⊙). Magenta, red, yellow, green, cyan, blue, and gray points show the simulated results (magenta: α = 0.0, red: α = 0.4, yellow: α = 0.6, green: α = 1.0, cyan: α = 1.4, blue: α = 1.6, gray: α = 2.0).
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Relation between number of spatial pixels in clouds (N S) and radius (r) of clouds in the BKP catalog. The gray curve shows the result of the least-squares fitting (r = 0.25 ﹩\sqrt{{N}_{{\rm{S}}}}﹩ + 0.079) for clouds in the range of 5 ≤ N S ≤ 100.
Paper: Lyα Emitting Galaxies (LAEs) at Cosmic Dawn: Implications and Predictions
Authors: Eduard Salvador-Solé, Alberto Manrique, J. Miguel Mas-Hesse, Cristina Cabello, Jesús Gallego, José Miguel Rodríguez-Espinosa, Rafael Guzman
Figure caption: Visibility factor giving the best fit to the empirical estimates of f vis found by Konno et al. (2014; dots with error bars) in single (left) and double (right) reionizations (thick solid lines). Thin short-dashed and long-dashed lines give the solutions we would obtain if, instead of taking ﹩{s}_{\min }(z)\propto 1+z﹩ as found for ﹩{S}_{\min }=1.16﹩ pMpc, we take ﹩{s}_{\min }(z)\propto {\left(1+z\right)}^{2}﹩ and ﹩{s}_{\min }(z)﹩ constant, respectively, to mimic what could result from the dependence on other factors of the transmission of Lyα photons in neutral IGM. (At z ≲ 7.5, the dashed lines almost overlap with the solid ones in both reionization scenarios.)
Paper: Lyα Emitting Galaxies (LAEs) at Cosmic Dawn: Implications and Predictions
Authors: Eduard Salvador-Solé, Alberto Manrique, J. Miguel Mas-Hesse, Cristina Cabello, Jesús Gallego, José Miguel Rodríguez-Espinosa, Rafael Guzman
Figure caption: Redshift distribution of LAEs brighter than L Lyα  = 1043.5 erg s−1 per infinitesimal redshift as a function of z predicted in single (red line) and double (blue line) reionization compared to the histogram of real detections The latter has been rescaled so as to match the all-sky predictions in the most populated redshift bin centered at z = 8. The curve predicted in single reionization, which at that bin below overlaps with that predicted in double reionization, has been slightly shifted downwards for clarity. (A color version of this figure is available in the online journal.)
Paper: Lyα Emitting Galaxies (LAEs) at Cosmic Dawn: Implications and Predictions
Authors: Eduard Salvador-Solé, Alberto Manrique, J. Miguel Mas-Hesse, Cristina Cabello, Jesús Gallego, José Miguel Rodríguez-Espinosa, Rafael Guzman
Figure caption: Minimum UV luminosities (actually maximum MUV magnitudes in AB system) of visible LAEs in single reionization as a function of z (red lines) below which there should be no LAE in the single reionization scenario. We show the predictions for the favorite value of ﹩{f}_{\mathrm{esc},{\rm{G}}}^{\mathrm{ion}}=0.054﹩ (thick line), and the more conservative value of 0.1 (thin line). Dots mark the UV magnitudes of all LAEs detected at those redshifts, according to the estimates made by the corresponding authors (see the list in Section 1). This constraint does not hold in double reionization.
Paper: Lyα Emitting Galaxies (LAEs) at Cosmic Dawn: Implications and Predictions
Authors: Eduard Salvador-Solé, Alberto Manrique, J. Miguel Mas-Hesse, Cristina Cabello, Jesús Gallego, José Miguel Rodríguez-Espinosa, Rafael Guzman
Figure caption: Same as Figure 4 but for the Lyα luminosities corrected for ISM plus IGM absorption (thick solid lines) in single reionization (left panel) and double reionization (right panel). For comparison we show the original intrinsic Lyα LFs (thin solid lines) and after correction for ISM absorption only (thick dashed lines). Note that there is no thick solid orange line. (A color version of this figure is available in the online journal.)
Paper: Lyα Emitting Galaxies (LAEs) at Cosmic Dawn: Implications and Predictions
Authors: Eduard Salvador-Solé, Alberto Manrique, J. Miguel Mas-Hesse, Cristina Cabello, Jesús Gallego, José Miguel Rodríguez-Espinosa, Rafael Guzman
Figure caption: Minimum Lyα luminosity of LAEs in single reionization at very high z where ionized bubbles are carved by individual UV-bright galaxies. We show the results obtained from the best value of the escaping fraction of ionizing photons, ﹩{f}_{\mathrm{esc},{\rm{G}}}^{\mathrm{ion}}=0.054﹩, found in SS+17 (thick line), and a more conservative value of ﹩{f}_{\mathrm{esc},{\rm{G}}}^{\mathrm{ion}}=0.1﹩ (thin line).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Evolution of gas surface density in all models. The interval selected for computing the averaged tabulated quantities in each model is marked with a heavy curve.
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: Overview of the day surrounding the 5th perihelion of PSP. (a) Plasma density based on plasma frequency measurements. (b) Proton velocity. (c) Magnetic field. (d) The direction of the magnetic field, spherical angles θ   B   and ϕ   B  . The gray dashed lines mark the boundaries of the intervals favorable to near-f ce harmonic emissions: 80° < θ   B   < 100° and 10° < ϕ   B   < 30°. (e) Magnetic fluctuations spectrum. The white line represents the lower-hybrid frequency f LH. (f) Sum of the high-frequency AC electric field spectrum calculated from differential voltage data measured by V 12 and V 34 antennae pairs. The black line shows the proton plasma frequency f p and the white line represents the electron cyclotron frequency f ce. The white markers over the black background on the top of panel (f) mark the points in time where both θ   B   and ϕ   B   are inside their respective angular ranges favorable to near-f ce harmonic emissions as can be seen in panel (d).
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: High-cadence ∼3.5 s burst data showing a series of time-localized near-f ce harmonic wave emissions correlated with low-frequency magnetic field oscillations. (a), (b) Magnetic field in spacecraft coordinates. (a) B  z  and ∣B  z ∣. (b) B  x  (left axis) and B  y  (right axis). (c) Spherical angles: ϕ   B   (left axis) with the black dotted line marking the ϕ   B   = 30° boundary, and θ   B   (right axis) with the blue dotted line marking the θ   B   = 80° boundary. (d) Electric field waveform of the burst data. The two available components, E x  and E y , are in spacecraft coordinates. (e) Total electric field power spectrum. The white dotted line represents the electron cyclotron frequency.
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: The average intensity of near-f ce harmonic emissions as a function of the magnetic field direction. Data represent the entire day of 2020 June 7. Each dot corresponds to one spectral measurement averaged in the frequency range of the near-f ce harmonic waves, 1.8 kHz < f < 10 kHz. The magnetic field direction is characterized by θ   B   (vertical axis) and ϕ   B   (horizontal axis).
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: Near-f ce harmonic event showing a strong correlation between wave emission and variations in the magnetic field direction. Same panels as in Figure 2, see detailed description there. (a) Plasma density. (b) Solar wind velocity. (c) Magnetic field. (d) Spherical angles. (e) Magnetic fluctuations. (f) AC electric field spectrum.
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: Zoomed in figure of the near-f ce harmonic event shown in Figure 4. Shown are only the bottom four panels of Figure 4. (a) Magnetic field, (b) spherical angles, (c) magnetic fluctuation spectrum, and (d) AC electric field spectrum.
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: RTN coordinate system and angles used in the study. The magnetic field vector (red arrow) represents a characteristic situation when the magnetic field is close to radial and points sunward, such as during PSP’s 5th perihelion. The two angles shown are ﹩{\theta }_{{\boldsymbol{B}}}=\arccos ({B}_{N}/| {\boldsymbol{B}}| )﹩ (in blue), the polar angle of  B  with respect to  N , and ﹩{\phi }_{{\boldsymbol{B}}}=\arctan ({B}_{T}/{B}_{R})﹩ (in green), the azimuthal angle between the projection of the magnetic field vector onto the RT plane and the line parallel to the  R  direction.
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: Near-f ce harmonic event from 2021 January 16 (orbit 7), showing the same correlations between the magnetic field direction and the high-frequency electric field wave emissions. (a) Plasma density. (b) Solar wind velocity. (c) Magnetic field. (d) Spherical angles. (e) Magnetic fluctuations. (f) AC electric field spectrum.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Iterative exploration and optimization of the input parameters (left) and how the goodness-of-fit parameter changes during this optimization (right).
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Illustration of the oct-tree construction for determining which bubbles a halo lies inside of. The colors represent the levels (black: first level; blue: second level; orange: third level). The bubbles (circles) are colored according to the node they are associated with. Each bubble is associated with the smallest tree node it is completely contained within.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Redshift evolution of M crit in our fiducial (S21) model and two other models, computed for several different values of the streaming velocity: v BC = 0, 0.8, 2, and 3 times σ rms. The values of M crit in the OHS, S21, and F13 models are plotted in green, red, and blue, respectively. We additionally plot M ACH in gray for reference.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Correlations between the input parameters (horizontal) and goodness-of-fit parameters (vertical) for 128 randomly chosen combinations of input parameters. This plot illustrates which observables are sensitive to which input parameters.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Disk mass (estimated from the total dust continuum flux) of the compact sources detected with ALMA long-baseline observations (see Table 2) as a function of their projected distances from the massive stars. Here, for any source, we calculate its distances to sources 1 and 2, and use the smaller value as its distance from massive stars. For sources 1−4, free–free emission is subtracted from the continuum (see Table 2 and Section 5). (b) Distribution function of separations between the ALMA sources. The quantity p(s)Δs (area under the curve) is the number of pairs of sources with their separation falling within the range [s, s + Δs]. Separation s is normalized to the cluster radius(18.″1, 4.0 × 104 au), which is determined by the maximum separation between any source to the average position of all the sources. (c) MST for the ALMA sources. The position offsets are with respect to the position of source 2. The stars mark the four massive sources with corresponding VLA detection (sources 1−4). The cross marks the average position of all the sources. (d) Mass segregation ratio parameter ΛMSR (see text) as a function of the number of most massive sources. The black data points and curve show ΛMSR calculated with sources ordered by their disk masses. The red data points and curve show ΛMSR calculated by setting the four sources with VLA detections (sources 1−4) to be the most massive ones (ordered by their estimated stellar mass), followed by the other sources ordered by their disk masses. The two outermost sources are not included as the low primary beam response near the edge of the field of view biases toward relatively bright and therefore massive sources. The two sets of data points are offset slightly on the x-axis for better presentation. The dashed line shows ΛMSR = 1 indicating no mass segregation.