adsabs/AstroCLIMB huggingface dataset:
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Clustering statistics of critical points: redshift evolution at fixed rarity threshold (﹩{ \mathcal R }=20﹩) and within a given cosmological framework. Top panels are for the baseline massless neutrino model, in the middle panels M  ν  = 0.1 eV, and bottom panels display M  ν  = 0.4 eV. In each panel, contrasting colors represent different redshifts (z = 1, 2, 3)—as specified by the inset. While at intermediate r-separations all of the autocorrelations show little evolution with redshift, in general, even if small, z-evolution is more relevant for the correlations involving the most nonlinear critical points (i.e., extrema).
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Spatial positions of the inflection points of the autocorrelation functions at large scales for three different cosmologies, as inferred from Figure 6, ordered by critical point type (from top to bottom: minima, wall-type saddles, filament-type saddles, maxima). Red squares denote M  ν  = 0.0 eV, blue triangles are used for M  ν  = 0.1 eV, and green circles show M  ν  = 0.4 eV, at z = 0. Gray horizontal error bars indicate ±0.1% variations in ξ. A clear remarkable trend is seen as a function of neutrino mass.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Critical point pair cross-correlations: determination of the corresponding inflection scales in the interval 110 h −1 Mpc < r < 140 h −1 Mpc, from averages over 100 independent QUIJOTE realizations per cosmology at z = 0, as specified in the panels. From left to right, ﹩{ \mathcal P }{ \mathcal V },{ \mathcal P }{ \mathcal W },{ \mathcal V }{ \mathcal F },{ \mathcal W }{ \mathcal F },{ \mathcal P }{ \mathcal F },{ \mathcal V }{ \mathcal W }﹩ are shown, for three rarity thresholds (﹩{ \mathcal R }=5,10,20﹩) represented by contrasting colors. Shaded horizontal error bars display the levels where ξ varies by ±0.1%. In all of the panels, vertical gray dashed lines indicate the exact positions of the inflection scales, highlighting their sensitivity to neutrino mass effects.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: BAO dip/peak amplitudes (r 2 ξ) at z = 0, vs. their correspondent spatial positions (r = 102.5 h −1 Mpc, independent of critical point type pair, neutrino mass, and rarity), inferred from the cross-correlation measurements presented in Figures 8 and 9. From top to bottom, ﹩{ \mathcal P }{ \mathcal V },{ \mathcal P }{ \mathcal W },{ \mathcal V }{ \mathcal F },{ \mathcal W }F,{ \mathcal P }{ \mathcal F },{ \mathcal V }{ \mathcal W }﹩ are shown. Different colors indicate distinct cosmologies, while contrasting symbols represent three choices of rarity thresholds. A clear trend as a function of neutrino mass can be readily inferred.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Inflection scales of critical point pairs, inferred via ﹩{ \mathcal P }{ \mathcal V }﹩, ﹩{ \mathcal P }{ \mathcal W }﹩, ﹩{ \mathcal V }{ \mathcal F }﹩, ﹩{ \mathcal W }{ \mathcal F }﹩, ﹩{ \mathcal P }{ \mathcal F }﹩, and ﹩{ \mathcal V }{ \mathcal W }﹩ cross-correlation measurements at z = 0 (from top to bottom). Red squares indicate M  ν  = 0.0 eV, blue triangles are for M  ν  = 0.1 eV, and green circles denote M  ν  = 0.4 eV. Shaded horizontal error bars highlight ±0.1% variations in ξ; all of the inflection point spatial positions fall within this range.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: BAO dip/peak amplitudes in massive neutrino cosmologies obtained from cross-correlation measurements, normalized by their correspondent values in a massless neutrino scenario and expressed in percentages as a function of rarity threshold at z = 0 (with ﹩{ \mathcal R }=5,10,20﹩, respectively). Colors and symbols are the same as in Figure 5. In cross-correlations, departures from analogous measurements carried out in the baseline M  ν  = 0.0 eV framework can be as high as ∼9% at z = 0 when M  ν  = 0.1 eV.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Clustering statistics of critical points: redshift evolution at fixed rarity threshold (﹩{ \mathcal R }=20﹩) and varying cosmologies (red lines: baseline massless neutrino model; blue lines: M  ν  = 0.1 eV; cyan lines: M  ν  = 0.4 eV). Top panels are for z = 1, middle panels refer to z = 2, and bottom panels are for z = 3. Minima, wall-type saddles, filament-type saddles, and maxima are represented—from left to right.
Paper: Signature of Massive Neutrinos from the Clustering of Critical Points. I. Density-threshold-based Analysis in Configuration Space
Authors: Jeongin Moon, Graziano Rossi, Hogyun Yu
Figure caption: Critical point autocorrelation tests related to the bin size choice (left) and to the selection of the smoothing scale (right). In both panels, we consider only maxima at z = 0 for a rarity ﹩{ \mathcal R }=5﹩ and the number of voxels N grid = 1024. In particular, altering the bin size does not affect the overall shape of the autocorrelation function (including the location of the BAO peak and the zero-crossing scale), while smoothing acts similarly to the effect of a rarity choice.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Mass and radius diagram of Hi-GAL compact sources corresponding to WGOs in each group. The black solid line shows a clear correlation between source radius and mass, ﹩{\mathrm{log}}_{10}(M/{M}_{\odot })=1.96{\mathrm{log}}_{10}(R/\mathrm{pc})+4.18﹩. The red dashed line shows the sources which may form a high-mass star. The yellow dashed–dotted line indicates another higher threshold (Σcrit = 1g cm−2) for judging high-mass clumps. The deep yellow dashed–dotted line shows a lower threshold than the yellow one.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left: The 7 mm continuum emission toward 18345 is shown in white contours overlaid on the 1.3 cm color image from Rosero et al. (2016). The outlined and filled white ellipses in the bottom left represent the 7 mm and 1.3 cm synthesized beam sizes, respectively. The red circles and diamonds show the 6.7 and 44 GHz methanol masers from Beuther et al. (2002b) and Rodríguez-Garza et al. (2017), respectively. Right: SED of C 1. The black dots show the radio continuum data from Rosero et al. (2016), while the green square represents the 7 mm integrated flux obtained from the 2D Gaussian fit detailed in Section 3.1. The dashed gray and continuous blue lines show the power-law fit and ionized gas sphere model from Rosero et al. (2019), respectively.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: SiO integrated intensity in 18517 shown in color and black contours. The latter represent [−3, 3, 3.5, 4, 4.5] × σ SiO, with σ SiO = 18.1  mJy beam−1 km s−1. The white contours show the 7 mm emission and are the same as in Figure 1. The white cross marks the position of the radio continuum source. The filled, white ellipse in the bottom left represents the synthesized beam size. The SiO(1−0) emission is highly collimated and is clearly associated with the jet candidate embedded in the 7 mm core. The emission is monopolar and extends to about 0.08 pc from the 7 mm core. The green line was drawn to guide the reader on the possible direction of the emission.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: CS(1−0) integrated intensity map toward 18517 shown in color and black contours. The contour levels represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 600 and 147 mJy beam−1 km s−1, respectively. The white contours show the 7 mm emission and are the same as in Figure 1. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam sizes, respectively. The green line was drawn to guide the reader on the possible direction of the SiO emission and is the same as in Figure 3. The CS emission presents an elongated morphology in the north–south direction, although it is slightly asymmetric, more intense to the south. Its peak coincides with the 7 mm continuum peak.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: SiO × 5 and CS J = 1–0 emission in 18517 are shown in red and blue, respectively. The SiO and CS spectra were obtained by integrating over the entire emission that appears to be spatially connected to C 1 and enclosed in the 3σ and 35% contour levels from Figures 3 and 5, respectively. The SiO emission is highly asymmetric and shows a clear line wing toward blueshifted velocities. The CS line is single peaked and symmetric. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: The white contours show the 7 mm continuum emission toward 18517 C 1, and the 1.3 cm emission from Rosero et al. (2016) is shown in color. The filled and empty white ellipses in the bottom left represent the 1.3 cm and 7 mm synthesized beam sizes, respectively. We note that the centimeter and millimeter emission peaks are coincident. The red diamond and × show the position of the methanol 44 and 25 GHz emission from Rodríguez-Garza et al. (2017) and Sanchez-Tovar et al. (2022), respectively.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: SiO luminosity L SiO vs. bolometric luminosity L Bol (top) and 1.3 cm radio luminosity S  ν  d 2 (bottom) plots. The outlined square and circle show the luminosity values for 20293 C 1 if the near or far distance was adopted, respectively. Although the scatter in our data is significant, our observations suggest a positive correlation between L SiO and both L Bol and S  ν  d 2.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Spitzer IRAC color composite of 18517, showing the 3.6 (blue), 4.5 (green), and 8.0 μm (red) emission. The blue and magenta contours show the 7 mm continuum and SiO integrated intensity and are the same as in Figures 3 and 1, respectively. The black × marks the position of the radio continuum source. We note that the green band emission appears to be elongated at an angle of about 45° from the SiO outflow axis.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: SED of 18517 C 1. The black dots represent the 1.3 and 6 cm emission from Rosero et al. (2016), while the green square shows the 7 mm flux density. The error bar of the 7 mm flux density represents the Gaussian fit error plus 10% to account for calibration uncertainties. The solid, blue line and dotted, gray line represent the spherical ionized gas model and power-law fit from Rosero et al. (2019), respectively.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Top left: SiO(1−0) integrated intensity in 20293 shown in color and black contours. The latter represent the [−2.5, 2.5, 3.5, 4.5, 5.5, 6.5, 7.5] ×σ SiO levels, with σ SiO = 33.5  mJy beam−1 km s−1. The white contours show the 7 mm continuum emission and are the same as in the first panel of Figure A18. The white cross shows the position of the radio continuum source, and the white ellipse in the bottom left represents the synthesized beam size. Top right: CS(1−0) integrated intensity shown in color and black contours. The latter represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 600 and 62 mJy beam−1 km s−1, respectively. The white contours represent the 7 mm continuum emission and are the same as in the left panel. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam sizes, respectively. In both top panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow directions. Bottom: spectra of the SiO (×5) and CS J = 1–0 emission in 20293 shown in blue and red, respectively. These were obtained integrating over all the SiO emission to the southeast of the core and over all the CS emission enclosed by the 35% contour level shown in the top right panel. The vertical dotted line marks the systemic velocity. The red arrows were drawn to show the two CS peaks.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Top left:  SiO(1−0) integrated intensity map shown in color and contours. The latter represent the [−3, 3, 3.5, 4, 4.5, 5]  × σ SiO levels, with σ SiO = 12.9  mJy beam−1 km s−1. The white contours show the 7 mm continuum emission and are the same as in the left panel of Figure A16. The white cross shows the position of the radio continuum source, and the white ellipse in the bottom left represents the synthesized beam size. Top right:  CS(1−0) integrated intensity shown in color and black contours. The latter represent −25%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 260 and 69 mJy beam−1 km s−1, respectively. The white contours are the same as in the left panel, while the outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam sizes, respectively. In both top panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow directions. Bottom: spectra of the SiO (×5) and CS line emission associated with C 1 in blue and red, respectively. These were obtained integrating over the three SiO knots to the northeast of C 1 and over all the CS emission to the southwest of the core enclosed by the 25% contour level, as shown in the top right panel. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Top left: SiO(1−0) integrated intensity map shown in color and black contours. The latter represent the [−2.5, 2.5, 3, 4, 5, 5.5, 6]  × σ SiO levels, with σ SiO = 32.4  mJy beam−1 km s−1. The white contours show the 7 mm continuum emission and are the same as in the right panel of Figure A10. The white cross shows the position of the radio continuum source, and the white ellipse in the bottom left represents the synthesized beam size, respectively. Top left: CS(1−0) integrated intensity shown in color and black contours. The latter represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 676 and 166 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and are the same as in the left panel. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam sizes, respectively. In both top panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow directions. Bottom: spectra of the SiO (×5) and CS line emission in 19012 in blue and red, respectively. These were obtained integrating over the entire emission that appears to be connected with C 2. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1 but for 20293. The red square and diamonds mark the positions of the 22 GHz water and 44 GHz methanol masers from Beuther et al. (2002b) and Rodríguez-Garza et al. (2017), respectively. The SED of C 3 was created using the radio continuum flux of the ionized source 20293 C from Rosero et al. (2016), which contains the embedded component 20293 B. The scale bar marks ∼104  au because of the distance uncertainty of the region, which represents 104 and ∼15,000 au. Note the different color scales and contours used in each continuum image.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Spitzer IRAC color composite, showing the 3.6 (blue), 4.5 (green), and 8.0 μm (red) emission. The blue contours show the 7 mm continuum emission and represent the [2, 3, 4, 5, 7, 9, 11, 12.5]  × σ 7 mm levels, with σ 7 mm = 94.9  mJy beam−1. The magenta contours show the SiO integrated intensity and represent the [2.5, 3, 4, 5, 5.5,6] ×σ SiO levels, with σ SiO = 32.4  mJy beam−1 km s−1. The black × marks the position of the radio continuum source.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1, but for G53.11.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left: CS(1−0) integrated intensity shown in color and black contours. The latter represent −15%, 25%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the CS moment-0 map being 846 and 181 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and represent [−3, 2.5, 3, 3.5, 5, 7, 9, 10]  × σ 7 mm, with σ 7 mm = 90.7 μJy beam−1. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam size, respectively. Right: spectrum of the CS line emission in 19266, obtained integrating over the entire emission enclosed in the 35% contour level from the left panel. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as in the left panel of Figure A1, but for 19266. Note the different color scales and contour levels used in each panel.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: SED of the cores in 19266 with centimeter counterpart. The black circles and green square represent the 1.3/6 cm data from Rosero et al. (2016, 2019) and the 7 mm continuum emission, respectively. The gray dashed line shows the power-law fit applied to the radio continuum emission.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Same as Figure 5 but for R9. This is a large disk (﹩{r}_{\max }=13﹩                      M) with a relativistic adiabatic index ﹩\hat{\gamma }=4/3﹩. The filled region near the polar axis indicates that a relativistic jet is not formed.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Time and azimuthal angle (ϕ) average location in the z − θ plane of the σ = 1 surface (plotted by the thick black line in Figures 5 and 6) for runs R2 and R3. Both runs have a similar initial setup, differing only by the value of the adiabatic index (﹩\hat{\gamma }=4/3﹩ in R2 and ﹩\hat{\gamma }=5/3﹩ in R3). A larger adiabatic index results in higher gas pressure inside the disk, making the resulting jet narrower. The vertical black line marks the outer horizon radius.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Time evolution of the barycentric radius for four runs with different initial magnetizations: R1 and R2 (β 0 = 100), R7 (β 0 = 44), and R8 (β 0 = 20). The maximum integration radius ﹩{r}_{\max }=80﹩                      M is taken in all calculations (see Equation (48) and the following discussion). The increase in the barycentric radius is due to viscous spreading. Clearly, the larger the initial magnetic field (the smaller the β 0) the faster the disk expands, implying that the initial viscosity is directly related to the initial magnetization, β 0.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Comparing the effects of varying the resolution. Left: comparison between R1 and R2. Right: comparison between R5 and R6. From top to bottom: Density, poloidal velocity u  ϕ , gas pressure p  g , plasma β, and disk width H. The thick lines are averaged over time such that 5 × 103M < t < 104M and the shaded regions correspond to the maximal variation amplitude for data exported every Δt = 5M.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Same as Figure 4 but for R5 and R6. Left: time-averaged mass accretion rate as a function of radius r for different time intervals. Right: time-averaged angular momentum flux as a function of radius. The pink region corresponds to the 2σ variance during the last time interval, 8000M < t < 104M. From this figure, it is clear that at the end of our run, a quasi-steady state is not achieved.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Same as Figure 5 but for R7 (top) and R8 (bottom). They differ by the initial value of β 0.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Left: Time-averaged mass accretion rate ﹩\dot{M}﹩ for runs R1, R2, R7, and R8, which only differ by their value of β 0. Error bars represent 2σ variance. Right: same but for the MAD parameter Φ B .
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Barycentric radius for the two nonequilibrium simulations. For both simulations, the disk initially contracts, bounces two times, and then starts expanding in a similar manner to the other disks, which start from an equilibrium state.