adsabs/AstroCLIMB huggingface dataset:
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: Quasar-host decomposition of NIRCam/F356W images for all 12 targets. The rows are as follows from top to bottom: (1) original science image (data), (2) data minus quasar model, i.e., the host galaxy and neighbors, (3) best-fit host Sérsic model(s), and (4) SNR maps of the host significance; the noise is a combination of that from the data and the scatter of the corresponding top five PSFs. In row (4), we show the elliptical apertures within which we calculate the host SNR, as reported in Table 2. When drawing these apertures, we use solid lines to highlight those with confirmed host detections. The inferred host-to-total flux ratios from the best fit are also indicated in the bottom panels. Our simulation results indicate that even in challenging cases, such as J0844−0132, we are able to accurately recover the host galaxy properties, as demonstrated in Figure 9.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: Host-to-total flux ratio as a function of the quasar’s absolute magnitude. The plot includes three luminous z ∼ 6 quasars reported in M. Yue et al. (2024). Our results demonstrate that the intrinsically low luminosity of our quasars leads to a significantly higher host-to-total flux ratio than found in luminous quasars. Note that the photometric measurements of the host galaxies in M. Yue et al. (2024) are based on a different methodology that results in very small statistical uncertainties, leading to exceptionally small error bars in their sample. The 3% threshold, which serves as one of our detection criteria for hosts, is indicated by the dashed line.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: The redshift-M1450 distribution of the SHELLQs quasars in this study (red) and other major JWST observations for luminous quasars: EIGER (blue; M. Yue et al. 2024) and ASPIRE (orange; F. Wang et al. 2023). The SHELLQs quasars, whose host detections were reported in our earlier papers (X. Ding et al. 2023; M. Onoue et al. 2024) are indicated by larger open circles.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: Same as Figure 2 for the F150W filter. Note that for nonsignificant detections (i.e., those indicated by dashed-line elliptical apertures), the inferred host properties have larger uncertainties. In these cases, the orientation of the inferred host shape in F150W can even be inconsistent with that in F356W.
Paper: SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6
Authors: Xuheng Ding, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, Knud Jahnke, Camryn L. Phillips, Tommaso Treu, Irham T. Andika, Kentaro Aoki, Junya Arita, Shunsuke Baba, Sarah E. I. Bosman, Anna-Christina Eilers, Seiji Fujimoto, Zoltan Haiman, Masatoshi Imanishi, Kohei Inayoshi, Kazushi Iwasawa, Jeyhan Kartaltepe, Nobunari Kashikawa, Toshihiro Kawaguchi, Junyao Li, Chien-Hsiu Lee, Alessandro Lupi, Jan-Torge Schindler, Malte Schramm, Kazuhiro Shimasaku, Marko Shuntov, Takumi S. Tanaka, Yoshiki Toba, Benny Trakhtenbrot, Hideki Umehata, Marianne Vestergaard, Feige Wang, Jinyi Yang
Figure caption: (a) This figure presents the SED inference for our host galaxies, derived using the GSF software. Red data points with error bars represent the inferred host galaxy fluxes across multiple bands. The gray-shaded region illustrates the 1σ range of SED template variations obtained through MCMC sampling. The black line denotes the median SED template. Blue diamonds indicate the flux predictions based on this median template for each observed band. We use eight-band photometry to infer the SED for J2236+0032 (M. Onoue et al. 2024). (b) For J1146−0005, the inferred host detection in F356W is weak and does not pass the detection criteria. Thus, the inferred stellar mass for this target should also be considered as an upper limit.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Scenario 1: PW→CW(γ) Maximum (panel (a)) and minimum (panel (b)) gamma-ray flux from a typical RB (red bands) and BW (black bands). All the curves are calculated assuming that protons are injected as a delta function. The solid (dashed) lines are obtained for ﹩\dot{E}=1{0}^{35}\,{{\rm{erg}}}\,{{{\rm{s}}}}^{-1}﹩ (﹩\dot{E}=1{0}^{33}\,{{\rm{erg}}}\,{{{\rm{s}}}}^{-1}﹩). The bands include the uncertainty in the magnetic field in the companion region Bc. The upper (lower) bound is obtained assuming Bc = 103 G (Bc = 0.1 G). The maximum is obtained by calculating the multiplicity according to Equation (18) The minimum is obtained assuming a fixed multiplicity of 104. The dashed and dotted–dashed orange lines represent the 50 hr CTA sensitivity in the north and south hemispheres, respectively (S. Celli & G. Peron 2024). The blue solid line represents the 1 yr LHAASO sensitivity (S. Celli & G. Peron 2024).
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Scenario 2: IBS→CW(γ) Maximum for gamma-ray flux from a typical RB (red lines) and BW (black lines). All the curves are calculated assuming ηp = 0.8 and that protons are injected as a power-law with an exponential cut-off, where the spectral index is fixed to α = 1.5 (panel (a)) and α = 2.5 (panel (b)) and the cut-off energy is fixed to 300 TeV, calculated according to Equation (14). The bands include the uncertainty in the magnetic field in the companion region Bc. The upper (lower) bound is obtained assuming Bc = 103 G (Bc = 0.1 G).
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Sketch of a spider system. The MSP is represented as a blue sphere on the left (not to scale), while the CS is shown as a yellow sphere on the right. The pulsar (companion) wind is indicated with blue (yellow) arrows. The interaction between the winds forms the IBS, depicted as a blue semicircle. (a) The green hollow cylinder around the companion represents the interaction region of protons with the CW. (b) The green cylinder around the companion represents the interaction region of protons with the CS.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Scenario 1: PW→CS(ν) Same as in Figure 4 but for the all-flavor neutrino flux. The 90% confidence-level median sensitivities of the IceCube (blue band) (M. G. Aartsen et al. 2020), KM3Net-ARCA (orange band) (S. Aiello et al. 2019), and TRIDENT (green band) (Z. P. Ye et al. 2023) detectors, based on 10, 6, and 10 yr of data-taking, respectively, are shown assuming a power-law source spectrum with an index of 2. The exact sensitivity value will depend on the decl. of the considered source.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Timescales for the interaction of protons with the CW (panel (a)) and with the CS (panel (b)). The diffusion, pp, and ballistic timescales are displayed with colored-shadowed bands, and dashed, dashed–dotted lines, respectively. Timescales for typical RBs (BWs) are displayed in red (black). The uncertainty in τdiff is due to the uncertainty in the magnetic field in the companion region. The lower part of the band is obtained assuming Bc = 0.1 G, while the upper part is obtained for Bc = 103 G.
Paper: Very High-energy Gamma-Ray and Neutrino Emission from Hadronic Interaction in Compact Binary Millisecond Pulsars
Authors: V. Vecchiotti, M. Linares
Figure caption: Histogram of the spin-down power for RBs (red), BWs (black), and RBs plus BWs (white) in Tables 2 and 3 with known spin-down power.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Similar to Figure 11 but on X-class flares.
Paper: Systematic Nonthermal Velocity Increase Preceding Soft X-Ray Flare Onset: A Large-scale Hinode/EIS Study
Authors: Andy S. H. To, Abigail Burden, Deborah Baker, Henrik Eklund, David H. Brooks, Laura A. Hayes, Juan Martínez-Sykora, Paola Testa, Jeffrey Reep, Miho Janvier, Shinsuke Imada, Julio Hernandez Camero, David M. Long, Teodora Mihailescu, Micah J. Weberg
Figure caption: Similar to Figure 11 but on C > 4 class flares.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: (a) Velocity-integrated intensity (moment 0) map of 12CO J = 2–1 emission with intensities greater than 3 σCO (σCO = 3.8 mJy beam−1) in the velocity ranges of 4.6–7.6 km s−1 and 7.8–12.8 km s−1. (b) Velocity-field (moment 1) map of 12CO J = 2–1 emission. The plot area is limited to the region larger than 4.5 × 10−3 arcsec2. The velocity of 0 km s−1 corresponds to the central velocity vcent = 7.7 km s−1. The contours in panels (a) and (b) represent the 1.3 mm continuum emission from the SpM image shown in Figure 1(b), with contour levels of 0.03, 0.05, and 0.08 Jy arcsec−2. (c) Position–velocity diagram along the position angle (PA) of the dust disk, from south to north. The offset of 0 au corresponds to the position of the star. The white dashed and solid curves represent the Keplerian rotation for the stellar mass M* = 0.7 M⊙ and 1.0 M⊙, respectively. Note that these curves are corrected for the inclination angle of dust disk idisk.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: (a) The uv coverage of the ALMA observation toward IRAS 04125+2902 with the configurations of C-6 and C-7. The region within the red dashed circle, with a radius of 1.2 Mλ, indicates the data set used for the axisymmetric disk modeling described in Section 4.1. (b) Disk model image created using the best-fit values of ﹩\cos i﹩ and PA, assuming an axisymmetric disk. (c) Residual map generated by applying tclean to the data set obtained after subtracting the model visibility from the observed visibility. The black contours represent the 1.3 mm continuum emission from the SpM image shown in Figure 1(b), with contour levels of 0.03, 0.05, and 0.08 Jy arcsec−2.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Results of the disk modeling based on M. Aizawa et al. (2024) applied to four different data sets: full-baseline observation visibility (first column), and visibility limited to baselines of 1.5 Mλ (second column), 1.2 Mλ (third column), and 1.0 Mλ (fourth column). From top to bottom, the panels show the intensity profiles of the best-fit disk model images, the real and imaginary parts of the observation and model visibilities, and two-dimensional images created from the intensity profiles assuming an axisymmetric disk displayed with the same color scale. In the visibility plots, black markers indicate the observed visibilities binned into 107 bins with a width of 20 kλ from 0.1 λ to 2.3 Mλ, while red lines represent the model visibilities.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Same as the left panels of Figure 2, but for the radial intensity profile averaged over the full azimuthal angle of the 1D brightness model shown in Figure 6(b). The dotted yellow lines show the profiles of the 1D brightness model image smoothed with the effective spatial resolution θeff by the CASA task imsmooth.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: (Top) Two RADMC model images. Note that these images were convolved with a Gaussian beam of the same size as the effective spatial resolution θeff of the SpM image. (Bottom) Peak intensity profile in the azimuthal direction. Note that all the profiles were created after the deprojection. All the profiles in both the top and bottom panels are linearly interpolated onto radial grid points spaced by 0.1 au using interpolate.interp1d from the SciPy module.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: Evolution of the spin parameters of PSR B1509–58. Panel (a): The evolution of ﹩\ddot{\nu }﹩. It decreases over time and displays significant variations, particularly around MJD 54000. Panel (b): The evolution of the braking index n. The blue square points after MJD 54600 are obtained in this work, while the black circle and diamond points before MJD 54600 are reported by M. A. Livingstone et al. (2005) and M. A. Livingstone & V. M. Kaspi (2011).
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Corner plot of the posterior distribution for six parameters (﹩{\rm{\Delta }}{x}_{{\rm{cen}}},\,{\rm{\Delta }}{y}_{{\rm{cen}}},\,\cos i,\,{\rm{PA}},\,\gamma ,\,\alpha ﹩) obtained from the axisymmetric disk modeling applied to the visibility data of the dust continuum emission around IRAS 04125+2902. The most probable parameter values are displayed at the top of the histogram panels.
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Same as Figure 1, but we adopted the same color scale as the SpM image for the CLEAN image.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The broadband high-energy spectrum of PSR B1509–58, including 0.5–2 keV. Panel (a): The phase-averaged spectrum. Panel (b): The phase-resolved spectra for three different phase intervals. The triangle, diamond, square, and cross points represent the data from NICER, Insight-HXMT/ME, Insight-HXMT/HE, and Fermi/LAT data in both panels. The solid lines represent the SuperExpCutoffPowerLaw model.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: Pulse profiles (50 bins; arbitrary phase) observed by Insight-HXMT/HE (30–150 keV), Fermi/GBM-NaI (30–150 keV), respectively. The red dashed lines are the fitting results, while the black dashed lines represent the Gaussian components. The shape and the fitting result of the two profiles are consistent within error.
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Effect of the central luminosity Lcenter = 5, 20, 100L⊙ (from left to right) on the evolution of adisr,dynamic (first three columns) and ﹩{a}_{{disr},{\rm{\max }},{\rm{dynamic}}}﹩ (next three columns) with vgas and nH inside the jet and outflow after 1, 5, 20, and 100 yr (from top to bottom). The color bars for the first three columns expands from 0.5 to 20 μm, and the color bars for the next three columns ranges from ∼20 to ∼500 μm. Gray squares indicate areas unaffected by RATD. Grains with ﹩{S}_{{\rm{\max }}}=1{0}^{3}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩ can start being destroyed by RATD inside the jet/outflow base after ∼1 yr even for Lcenter = 5L⊙ (Figure 10(a)). The outflow area enriched with the high abundance of small grains induced by RATD expands outward with time. The disruption size range is broadening with increasing Lcenter.
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Variation of the maximum size with fhigh-J = 0.5, ﹩{a}_{{\rm{\max }},{\rm{JB}}}^{{\rm{DG}},0.5}﹩ (upper row) and fhigh-J = 1, ﹩{a}_{{\rm{\max }},{\rm{JB}}}^{{\rm{DG}},{\rm{1}}}﹩ (lower row) with ﹩{n}_{{{\rm{H}}}_{2}}﹩ and vgas on outflow scales of 600 × 800 au. The left, middle, and right columns show results obtained for SPM grains with Ncl = 102, 103, 104 iron atoms/clusters. Dust grains within the disruption size range inside the outflow cavity can have perfect alignment with B and perfect disruption by RATD if grains are SPM with Ncl ≥ 103. The disruption fraction decreases with decreasing Ncl and is smaller inside the jet lobe, the outflow cavity wall, and inner envelope.
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Spatial distribution of the minimum disruption size adisr,POLARIS obtained from POLARIS with different values of ﹩{S}_{\max }=1{0}^{3}-1{0}^{7}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}﹩, from left to right, respectively. We show results on the slice containing the sink particle, with the spatial scale of 2000 au around the protostar. The empty region illustrates the area without RATD activities. The disruption happens strongest inside the outflow cavity due to lower gas densities, with adisr,POLARIS ∼ 0.5 μm for grains with ﹩{S}_{{\rm{\max }}}=1{0}^{3}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩ and higher adisr,POLARIS ∼ 5 μm for grains with ﹩{S}_{{\rm{\max }}}=1{0}^{7}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩. The RAT disruption only happens inside the inner envelope or the outflow cavity wall when grains are highly porous with low ﹩{S}_{{\rm{\max }}}\,\leqslant \,1{0}^{5}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩. This mechanism cannot affect dust grains on the equatorial midplane due to the high dust reddening effect along this direction and additional damping of RAT efficiency by the perpendicular between the radiation and magnetic field there.
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Effect of Lcenter on the time-evolution of adisr,dynamic and ﹩{a}_{{disr},{\rm{\max }},{\rm{dynamic}}}﹩ for grains with ﹩{S}_{{\rm{\max }}}=1{0}^{4}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩ with vgas and nH. The panel setups are similar to Figure 10. RATD can destroy grains with ﹩{S}_{{\rm{\max }}}=1{0}^{4}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩ inside the outflow base within ∼1 yr even when Lcenter = 5L⊙ (Figure 13(a)). Dust grains spanning from adisr,dynamic ∼ 4–5 μm to ﹩{a}_{{disr},{\rm{\max }},{\rm{dynamic}}}\sim 100\,\mu {\rm{m}}﹩ can be removed from ∼800 au scale of the outflow cavity if protostars hold Lcenter = 5L⊙ for over ∼100 yr (Figures 13(s) and (v)).
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Spatial distribution of the power index α of the size distribution of small grains below adisr,POLARIS on scales of 2000 au. Grains inside the region unaffected by RATD (empty regions in Figure 15) have the standard power index α = −3.5 of the MRN distribution, while small grains in the active region of RATD will have higher negative α due to the fragmentation of large grains beyond adisr,POLARIS (shown in Figure 15) to smaller sizes. The abundance of small grains increases, i.e., larger negative α, inside the jet and outflow cavity during the RATD period, and η will become more negative with decreasing ﹩{S}_{{\rm{\max }}}﹩. Small grains can be slightly enhanced inside the outflow cavity wall and inner envelope if grains have ﹩{S}_{{\rm{\max }}}\,\leqslant \,1{0}^{4}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩.