adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Photon–photon annihilation optical depth for 1 TeV photons. The purple line shows the optical depth to photon–photon annihilation for photons of 1 TeV observed energy produced in the forward shock downstream as a function of the observed time after the gamma-ray trigger. The bands show the 50% (darker band) and 90% (lighter band) uncertainty propagated from the modeling uncertainties. The vertical dashed lines show the times of the HESS observations, namely, 5 (blue) and 30 (red) hr.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Bulk Lorentz factor. Shown is the correlation between the gamma-ray isotropic equivalent energy and the bulk Lorentz factor for 67 long GRBs (red circles) and one short GRB (green square). The yellow star shows GRB 190829A. Lower limits on Γ0 are also shown (black arrows). The data are from Ghirlanda et al. (2018). The solid line shows the power law that best fits the red points.
Paper: The Universe is Brighter in the Direction of Our Motion: Galaxy Counts and Fluxes are Consistent with the CMB Dipole
Authors: Jeremy Darling
Figure caption: VLASS (left) and RACS (right) catalog sources in galactic coordinates. Darker color indicates fewer sources. ∣b∣ < 5° was excluded from the VLASS.
Paper: The Universe is Brighter in the Direction of Our Motion: Galaxy Counts and Fluxes are Consistent with the CMB Dipole
Authors: Jeremy Darling
Figure caption: Mean VLASS and RACS areal density vs. R.A. (left) and declination (right) in 5° increments. The vertical dotted lines denote the declination cuts used for the single-survey dipole fitting (δ > −15° for the VLASS and δ < +25° for the RACS), and the horizontal dotted lines indicate the median values. The vertical black line shows the declination where the two surveys are cut for the joint analysis. The lower source density seen in the VLASS vs. R.A. is caused by the falloff in source counts for δ < −15°. When the indicated declination cut is applied, the source density in the VLASS matches that of the RACS.
Paper: The Universe is Brighter in the Direction of Our Motion: Galaxy Counts and Fluxes are Consistent with the CMB Dipole
Authors: Jeremy Darling
Figure caption: Top: HEALPix maps of number counts (left) and integrated flux (right) for the scaled and combined surveys in galactic coordinates. The gray regions are masked. Middle: number (left) and flux (right) mean-subtracted maps smoothed to 1 sr. These maps should not be confused with fractional difference maps, which are unitless. Bottom: spherical harmonic fit velocity maps for number (left) and flux (right). The blue and red points indicate the apex and nadir of the CMB dipole (Planck Collaboration et al. 2020a, 2020b).
Paper: The Universe is Brighter in the Direction of Our Motion: Galaxy Counts and Fluxes are Consistent with the CMB Dipole
Authors: Jeremy Darling
Figure caption: Left: dipole apex measured from radio source number counts (top) and fluxes (bottom) using the methods listed in Table 1. The star indicates the CMB dipole apex, and error bars are 1σ uncertainties. Right: dipole velocity measured from radio source number counts (top) and fluxes (bottom). The vertical line indicates the observed CMB dipole. The envelopes show the error distributions in dipole amplitudes, and the vertical tick marks show 1σ and 2σ uncertainties.
Paper: The Universe is Brighter in the Direction of Our Motion: Galaxy Counts and Fluxes are Consistent with the CMB Dipole
Authors: Jeremy Darling
Figure caption: VLASS (left) and RACS (right) catalog source count vs. peak flux density. The opaque color indicates the catalog selection regions prior to masking and trimming.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Source size upper limits and comparison with the model. In the middle panel, downward arrows show our 1σ, 2σ, and 3σ upper limits on the source size at each epoch (see Appendix A.4). The dashed lines show the source size evolution as predicted by our afterglow model (analytical t 5/8 scaling, Granot et al. 1999, in black; source size from our numerical model in red) assuming our best-fit parameters (see Appendix C.6). The pink shaded band shows the 90% credible interval implied by our afterglow parameter uncertainties. The surrounding smaller panels show previews of the cleaned radio maps for each epoch (full-size maps are available on Zenodo; see Salafia et al. 2022).
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Multiwavelength data and emission model. Circles represent X-ray fluxes (blue; values shown on the right axis) or flux densities (all other colors; values shown on the left axis) measured at the position of GRB 190829A at different times after the GRB trigger in several bands (see the legend). Optical flux densities have been corrected for both the Milky Way and host galaxy extinction, and the contribution of the host galaxy has been subtracted. The host galaxy contribution (Rhodes et al. 2020) has also been subtracted from the AMI-LA radio flux densities at 15.5 GHz. Stars mark the flux densities measured in our VLBI epochs. Solid lines of the corresponding colors show the predictions of our emission model including both the forward and reverse shocks. Dashed lines single out the contribution of the reverse shock emission. We interpret the initial plateau in the X-ray data as the superposition of the prompt emission tail and the rising reverse shock emission.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Constraint on the energy-to-density ratio. Blue, purple, and orange lines (same color coding as in Figure 1) show the posterior probability on ﹩\mathrm{log}(E/n)﹩ obtained (Appendix A.4) from the source size measurements (Appendix A.2) in our VLBI imaging epochs assuming the source to be a relativistic shock in self-similar expansion (Blandford & McKee 1976; Granot et al. 1999). The gray line shows the combined posterior from all epochs. The thin red solid line is the posterior obtained from fitting our forward-plus-reverse shock afterglow emission model to the available multiwavelength data.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Limit on the viewing angle from compactness arguments on the prompt emission. Shaded areas show the allowed regions on the (Γ, (θ view − θ jet)) plane, derived by the compactness limits A (photon–photon pair production), B (scattering off e ±), and C (scattering off e − associated with baryons). The solid black line (Γθ = 1) separates on-axis observers from off-axis ones. The green star marks the bulk Lorentz factor Γ value inferred from the afterglow light-curve modeling, while the purple star marks the parameters used in Sato et al. (2021). Both solutions are in the allowed region that ensures that the source is transparent to the observed high-energy prompt emission photons.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Predicted SEDs at the times of the HESS detections. We show with blue (red) solid lines our model at 5 hr (30 hr) after the gamma-ray trigger, with 90% and 50% credible bands in lighter shades. The HESS “butterflies” include the reported (Abdalla et al. 2021) systematic error contribution (summed in quadrature). We also show XRT butterflies at the corresponding times (from our own analysis; see Appendix C.3), plus GTC optical and NOEMA, ATCA, and AMI-LA radio data points taken at observing times lying within 0.2 dex.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Comparison between our shock dynamics and those from models in the literature. Red lines show the forward shock four-velocity (i.e., Γβ; solid), reverse shock four-velocity (dashed), and jet half-opening angle (dotted) as a function of the shock radius (in units of the Sedov length) as computed with our model for our best-fit parameters E 0 = 2.5 × 1053 erg, Γ0 = 57, and n = 0.21 cm−3. Blue lines show the same quantities computed following Granot & Piran (2012; their “trumpet” model) for the forward shock Lorentz factor and jet opening angle and Kobayashi (2000) for the reverse shock Lorentz factor.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Marginalized source size posterior probability density for simulated sources immersed in real noise. Solid curves, color-coded by the overresolution parameter (Martí-Vidal et al. 2012) ω = S/N(size/beam)2, show the marginalized posterior probability density of the source size (in units of the injected size) obtained by applying our MCMC-based fitting procedure to simulated circular Gaussian sources immersed in the noise of our October 3 VLBA 15 GHz observation. For ω ≳ 1, the source starts to be clearly distinguishable from a point source.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Comparison of the visibility amplitude dependence on the UV radius for a circular Gaussian and a relativistic blast wave (Granot et al. 1999). The circular Gaussian size has been adjusted to match the first peak of the blast wave; see text.
Paper: Multiwavelength View of the Close-by GRB 190829A Sheds Light on Gamma-Ray Burst Physics
Authors: Om Sharan Salafia, Maria Edvige Ravasio, Jun Yang, Tao An, Monica Orienti, Giancarlo Ghirlanda, Lara Nava, Marcello Giroletti, Prashanth Mohan, Riccardo Spinelli, Yingkang Zhang, Benito Marcote, Giuseppe Cimò, Xuefeng Wu, Zhixuan Li
Figure caption: Frequency-dependent shift of the initial reference point C from 5 to 15 GHz. The best-fit point-source models are plotted as green plus signs at 5 GHz and blue plus signs at 15 GHz. The contours show the 15 GHz image at the second epoch. Using the mean position of the optically thin, discrete, and compact jet component J1 as the reference point, the shift was derived and corrected in the joint astrometry.
Paper: Spectra of Magnetic Turbulence in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn
Figure caption: Cosine of the alignment angle ϕ  ℓ  between the magnetic and electric fluctuations in numerical simulations. The results are averaged over nine data cubes covering the indicated time intervals. The straight lines are shown for reference.
Paper: Spectra of Magnetic Turbulence in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn
Figure caption: Magnetic and electric spectra and total electromagnetic energy spectrum for two different magnetizations. The total energy spectrum approaches a k −3/2 power law at k ⊥ d  e  ≪ 1 and a k −3.5 power law at k ⊥ d  e  ≫ 1.
Paper: Spectra of Magnetic Turbulence in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn
Figure caption: Spectra of the normalized residual energy for two different magnetizations averaged over nine data cubes covering the indicated intervals of turnover times. The solid lines are shown for the reader’s reference.
Paper: When Do Stars Go Boom?
Authors: Harvey B. Richer, Roger E. Cohen, Jeremy Heyl, Jason Kalirai, Ilaria Caiazzo, Matteo Correnti, Jeffrey Cummings, Paul Goudfrooij, Bradley M. S. Hansen, Molly Peeples, Elena Sabbi, Pier-Emmanuel Tremblay, Benjamin Williams
Figure caption: Color–magnitude diagrams of the LMC cluster NGC 2164 in the WFC3 filters (F225W, F336W). In the left plot, the Padova isochrones are for ages of 60 (blue) and 100 (cyan) Myr and the CMD includes all stars that pass a mild error cut. The theoretical white dwarf cooling sequences (red) are for masses 0.9–1.3 in steps of 0.1 M ⊙. The right plot, with the same isochrones and cooling models, additionally requires the stars to be present in our F814W images. There are no red giants here as they are saturated in the F814W exposures.
Paper: When Do Stars Go Boom?
Authors: Harvey B. Richer, Roger E. Cohen, Jeremy Heyl, Jason Kalirai, Ilaria Caiazzo, Matteo Correnti, Jeffrey Cummings, Paul Goudfrooij, Bradley M. S. Hansen, Molly Peeples, Elena Sabbi, Pier-Emmanuel Tremblay, Benjamin Williams
Figure caption: The diagrams in this figure explore the likelihood of the five potential NGC 2164 WDs being cluster members. The left plot is a blow-up around the WD cooling sequence of NGC 2164 and includes error bars in the photometry for the WDs, which are plotted in blue. The middle plot indicates the position of the five potential WDs on the sky (blue points) with respect to the cluster as well as a selection of bright cluster stars (green). The rightmost diagram illustrates contour diagrams for the completeness calculations.
Paper: When Do Stars Go Boom?
Authors: Harvey B. Richer, Roger E. Cohen, Jeremy Heyl, Jason Kalirai, Ilaria Caiazzo, Matteo Correnti, Jeffrey Cummings, Paul Goudfrooij, Bradley M. S. Hansen, Molly Peeples, Elena Sabbi, Pier-Emmanuel Tremblay, Benjamin Williams
Figure caption: Radial cumulative distribution for the different populations in the NGC 2164 and NGC 330 CMDs. In the left panel (NGC 2164), “White Dwarfs” consist of the five potential WD candidates, selected as absolute F225W magnitude fainter than +4 and color bluer than −1. The “Background Objects” are the 15 objects seen just to the red of the putative cluster WDs in the CMD of Figure 2 with colors between −1 and 0. “All Stars” contains all stars in the sample, and “Bright Stars” consists only of stars with absolute magnitude in F225W less than zero. The right panel shows the results of the same selections in the color–magnitude diagram for NGC 330.
Paper: When Do Stars Go Boom?
Authors: Harvey B. Richer, Roger E. Cohen, Jeremy Heyl, Jason Kalirai, Ilaria Caiazzo, Matteo Correnti, Jeffrey Cummings, Paul Goudfrooij, Bradley M. S. Hansen, Molly Peeples, Elena Sabbi, Pier-Emmanuel Tremblay, Benjamin Williams
Figure caption: Observed color–magnitude diagram of the globular cluster 47 Tucanae in the WFC3 filters F225W – F336W. The left y-axis (apparent F225W magnitude) is for 47 Tuc itself while the right y-axis moves the cluster to the distance of the LMC. The red line is a 1.0 M ⊙ WD cooling sequence for WDs in the LMC for temperatures from 100,000 to 30,000 K and illustrates that in these filters it should be possible to detect hot WDs at the distance of the LMC. The feature between the 47 Tuc WDs and the main sequence of the cluster is the upper main sequence of the LMC.
Paper: When Do Stars Go Boom?
Authors: Harvey B. Richer, Roger E. Cohen, Jeremy Heyl, Jason Kalirai, Ilaria Caiazzo, Matteo Correnti, Jeffrey Cummings, Paul Goudfrooij, Bradley M. S. Hansen, Molly Peeples, Elena Sabbi, Pier-Emmanuel Tremblay, Benjamin Williams
Figure caption: Color–magnitude diagrams of the two young LMC clusters (NGC 1805, NGC 1818) and the SMC cluster NGC 330 in the WFC3 filters (F225W, F336W). Padova isochrones (blue) for 25 and 40 Myr are shown for NGC 1805, 32 Myr for NGC 330, and 25 Myr for NGC 1818. The theoretical WD cooling sequences (red) are for masses 0.9–1.3 in steps of 0.1 M ⊙.
Paper: Probing the Origin of Cosmic Rays in Cygnus Cocoon Using Ultrahigh-energy Gamma-Ray and Neutrino Observations
Authors: Prabir Banik, Sanjay K. Ghosh
Figure caption: Left: the estimated differential EM SED reaching Earth from the Cygnus Cocoon in the leptohadronic origin scenario. The red dotted and green small-dashed lines represent the EM spectrum produced by synchrotron emission and Bremsstrahlung scattering of primary relativistic electrons in ambient matter, respectively. The EM spectrum produced by IC scattering of relativistic electrons with starlight fields around NGC 6910 and Cyg OB2, as well as a dust radiation field, is denoted by the gray long-dashed–single-dotted, magenta long-dashed–double-dotted, and violet long-dashed–triple-dotted lines, respectively. The gamma-ray flux created in pp interactions between relativistic protons and ambient protons is indicated by the brown small-dashed–single-dotted line. The black continuous line shows the estimated overall differential multiwavelength EM SED coming from the Cygnus Cocoon. The cyan very-long-dashed–single-dotted and orange very-long-dashed lines indicate the detection sensitivity of the LHAASO and e-ASTROGAM detectors for one years of observation, respectively. The blue long-dashed line represents our estimated gamma-ray flux limit detected by LHAASO. Right: the estimated corresponding all-flavor neutrino flux reaching the Earth from the Cygnus Cocoon.
Paper: Probing the Origin of Cosmic Rays in Cygnus Cocoon Using Ultrahigh-energy Gamma-Ray and Neutrino Observations
Authors: Prabir Banik, Sanjay K. Ghosh
Figure caption: The estimated relevant timescales for protons. The red dashed and magenta dashed–single-dotted lines represent the acceleration timescales with ξ  p  = 9 × 10−5 and 5 × 10−7 respectively. The blue dashed–double-dotted and green dashed–triple-dotted lines denote the energy loss timescale for protons in pp interaction and diffusion timescale respectively. The black continuous line indicates the lifetime of the Cocoon. The points, as indicated by the cyan and brown arrows, represent the maximum achievable energy by a cosmic-ray proton with ξ  p  = 9 × 10−5 and 5 × 10−7 respectively.
Paper: Probing the Origin of Cosmic Rays in Cygnus Cocoon Using Ultrahigh-energy Gamma-Ray and Neutrino Observations
Authors: Prabir Banik, Sanjay K. Ghosh
Figure caption: The estimated differential EM SED reaching Earth from the Cygnus Cocoon in the pure hadronic origin scenario. The black dashed–dotted and magenta dashed lines represent the EM spectrum produced with η  p  = 100%, α  p  = −2.6, and E  p,max = 5 × 1015 eV and η  p  = 1.6%, α  p  = −2.35, and E  p,max = 1014 eV, respectively. The blue continuous line represent our estimated gamma-ray flux limit detected by LHAASO.
Paper: Probing the Origin of Cosmic Rays in Cygnus Cocoon Using Ultrahigh-energy Gamma-Ray and Neutrino Observations
Authors: Prabir Banik, Sanjay K. Ghosh
Figure caption: The estimated relevant timescales for electrons. The red dashed and blue dashed–single-dotted lines represent the acceleration timescale of the electron with ξ  e  = 10−5 and synchrotron cooling timescale, respectively. The green dashed–double-dotted and magenta dashed–triple-dotted lines denote the diffusion and advection timescales, respectively. The points, as indicated by the cyan and brown arrows, represent the maximum achievable Lorentz factor and spectral break Lorentz factor of an electron, respectively.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from Their SiO Knots
Authors: Kai-Syun Jhan, Chin-Fei Lee, Doug Johnstone, Tie Liu, Sheng-Yuan Liu, Naomi Hirano, Ken'ichi Tatematsu, Somnath Dutta, Anthony Moraghan, Hsien Shang, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Shih-Ying Hsu, Woojin Kwon, Dipen Sahu, Xun-Chuan Liu, Kee-Tae Kim, Qiuyi Luo, Sheng-Li Qin, Patricio Sanhueza, Leonardo Bronfman, Zhang Qizhou, David Eden, Alessio Traficante, Chang Won Lee
Figure caption: Panels (a) to (f): CO (red color for redshifted and blue color for blueshifted) intensity maps and SiO (white contour) intensity maps for the six ALMASOP sources, G209 (HOPS 10), G205 (HOPS 358), G203, G191, G205S3 (HOPS 315), and G206 (HOPS 399). These maps have been rotated clockwise by 29°, 158°, 146.7°, −5°, −135°, and −20°, respectively, to align the jets with the vertical axis. For SiO, the contour levels start at 3σ with a step of 3σ, and σ are ∼0.02, 0.04, 0.01, 0.02, 0.03, and 0.06 Jy beam−1 km s−1 in panels (a) to (f), respectively. The green line segments indicate the SiO peak positions of the knots. The yellow-black stars denote the central source position. The green arrows mark the lengths of D obs and ΔD obs. Panel (g): Schematic diagram showing how fast and slow jet material interact to form the internal shocks seen as knots (Raga et al. 1990; Stone & Norman 1993; Suttner et al. 1997; Lee & Sahai 2004; Jhan & Lee 2016).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Deriving Inclination Angle and Velocity of the Protostellar Jets from Their SiO Knots
Authors: Kai-Syun Jhan, Chin-Fei Lee, Doug Johnstone, Tie Liu, Sheng-Yuan Liu, Naomi Hirano, Ken'ichi Tatematsu, Somnath Dutta, Anthony Moraghan, Hsien Shang, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Shih-Ying Hsu, Woojin Kwon, Dipen Sahu, Xun-Chuan Liu, Kee-Tae Kim, Qiuyi Luo, Sheng-Li Qin, Patricio Sanhueza, Leonardo Bronfman, Zhang Qizhou, David Eden, Alessio Traficante, Chang Won Lee
Figure caption: Panels (a) to (d): CO channel maps (contours) and C18O total intensity maps (color image) for the four ALMASOP sources G209 (HOPS 10), G205 (HOPS 358), G203, and G191. The contour levels start at 3σ with a step of 3σ, and the σ are ∼0.013, 0.016, 0.013 and 0.016 Jy beam−1 km s−1 in panels (a) to (d), respectively. The yellow-black stars denote the central source position. Panels (e) to (h): CO PV diagrams cut along the outflow axis for the four sources. The contour levels start at 10σ with a step of 10σ, and σ are ∼0.002, 0.0012, 0.001, and 0.002 Jy beam−1 in panels (e) to (h), respectively. The blue and red curves are the fits to the structures and PV structures of the outflows from the wind-driven shell model (see Section 3.2).