adsabs/AstroCLIMB huggingface dataset:
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The SFR and H I mass (M H I ) of our sample galaxies, compared with the average relation from star-forming nearby galaxies. (a) SFR vs. stellar mass M *. H I nondetections are indicated by empty gray dots; H I detections by WALLABY, FAST, and previous H I surveys are plotted as olive dots, orange circles, and blue dots, respectively. Estimations of lower limits of SFR are plotted as upward arrows in the corresponding color. All WALLABY detections have been covered by previous ALFALFA or HIPASS surveys, while FAST provides four new H I sources (orange filled circle). The stellar masses of H I-detected and -nondetected galaxies without SFR measurements are pointed out with bold and regular vertical salmon ticks, respectively. As a reference, the fitted local SFMS from Cook et al. (2014) is given as dashed gray line, and the scatter of 0.29 dex is given as the shaded region. The local SFMS of high-mass galaxies from Saintonge et al. (2016) is also plotted as the dashed–dotted gray line. The typical uncertainties of data points are plotted at the lower-right corner. (b) M H I  vs. M *. Most of the symbols are the same as those in panel (a). The upper limits of M H I  (dotted gray line) of H I nondetections (gray arrow) are provided, calculated with FAST or ALFALFA parameters according to their coordinates. Galaxies that only have lower limits of SFR are overlaid with gray crosses. The mean M H I  relation of local LTGs from Calette et al. (2018) is plotted as dashed gray line, with the extrapolated part of M * < 107 M ☉ translucent. Its scatter of 0.53 dex is given as shading. The typical uncertainties are also given.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The g − r color of H I-detected low-mass galaxies plotted against tidal strength S tid. The color is measured (a) using total fluxes, (b) at the galactic center, (c) at R 50, or (d) at 2R 50 (see Section 3.3 for details). Galaxies in the TS sample (f tid ≥ f RPS) are plotted as circles, color-coded as those in Figure 6. The size of circles represents stellar mass. For these galaxies, the Spearman correlation coefficient and the bisector fitting are given. The fitted line at R 50 is plotted in all other panels as bold gray lines for comparison. Remaining H I detections are plotted as gray dots, all of which are not involved in correlation calculation or fitting. The typical uncertainties for low-mass TS galaxies are given in panel (a).
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Additional effects of ram pressure P ram on the g − r color at 2R 50. Only galaxies whose predicted H I-disk sizes satisfy 1.5R H I  > 2R 50 are plotted, color-coded by the importance of P ram to the midplane gas pressure at 2R 50, i.e., ﹩{P}_{\mathrm{mid},2{R}_{50}}﹩. The size of the circles represents stellar mass. (a) The relation between the g − r color at 2R 50 and the ratio of H I mass density to stellar mass density at 2R 50. The bisector linear fitting result is plotted, and the slope is provided. The Spearman rank correlation and p-value of the relation are given with bootstrapped uncertainty. (b) The deviation of ﹩{(g-r)}_{2{R}_{50}}﹩ from the fitted relation in panel (a) vs. ﹩{P}_{\mathrm{mid},2{R}_{50}}﹩. A threshold of ﹩\mathrm{log}\left({P}_{\mathrm{mid},2{R}_{50}}/\mathrm{Pa}\right)﹩ (−14.18, vertical dotted gray line) is chosen to let samples above it have the strongest correlation. The Spearman correlation coefficient and the bisector fitting are given in dark purple. The correlation of galaxies below the threshold is listed in yellow.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The spatial distribution of gas stripping. H I detections and nondetections are plotted as filled and empty symbols, respectively. Irrelevant galaxies (i.e., their corresponding f = 0) in each panel are plotted as gray dots. Two dotted gray circles of radii 1 and 2 times R 200 indicate the range of N4636G, and the group center is labeled as a red cross. (a) The RPS strength map. Circles represent galaxies having gas strippable by ram pressure (f RPS > 0), color-coded by S RPS. The limits of the color bar are the 5th and 95th percentiles among all color-coded galaxies. (b) The tidal effect strength map. Galaxies having gas tidally strippable (f tid > 0) are plotted as diamonds, color-coded by S tid. The limits of the color bar are selected alike. (c) The stripping status map. Large colored symbols are those having strippable gas; blue circles are the RPS sample, and orange diamonds are the TS sample. They are color-coded exactly as those symbols in panels (a) and (b).
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Partial Spearman correlation coefficients r s for three g − r–S tid relations given in Figure 7. Orange slashed, green backslashed, and blue dotted bars correspond to the relation at R 50, at 2R 50, and of the whole galaxy, respectively. The controlled covariates are labeled along the x-axis. Only low-mass TS galaxies, i.e., colored symbols in Figure 7, are used. All of them have confident M H I  and SFR measurements. The p-values of these partial correlations are listed at the bottom of the figure, boldfaced ones smaller than 0.05. The threshold for strong correlation, ∣r s∣ = 0.45, is drawn as a gray dashed line.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: A reillustration of Figures 7(b)–(d). The g − r color of H I-detected low-mass galaxies is plotted against the position of color measurement, color-coded by the tidal strength S tid.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Different ICM density models for N4636G from the literature (see the legend) and the averaged ICM density profile (bold pink line). The pink shaded region indicates the uncertainty, considering the scatter of different models and the uncertainty of M gas,500 estimation. Historical X-ray surveys covered less than 20′ (vertical dotted gray line) from the group center. The R 500 and R 200 of N4636G are also drawn as vertical lines.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: This figure compares the accuracies of the GNN model with the analytic formulae obtained from symbolic regression and the modified equations using physical principles. Left: we first train a GNN with a compressed latent space representation to perform likelihood-free inference for the cosmological parameter Ωm with halo catalogs containing the positions and velocity moduli of the halos. Evidently, the model is able to achieve very high accuracy with a mean relative error of only ∼6.4% when evaluated on the test set of Gadget simulations. Despite its reduced dimensionality, this accuracy is comparable to the model found in Shao et al. (2022a). Right: we then use symbolic regression to extract analytic expressions for each MLP in the message-passing and final aggregation layers of the GNN. After modifying them to reduce their complexity and to preserve the symmetries of the model, we evaluate the expressions on the Gadget test set. As shown, the expressions are able to maintain the accuracy of the GNN, with an error of only ∼6.7%, indicating that the equations are close approximations for the learned GNN relations.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: This is a schematic of our methodology, which is explained in Section 3. We begin by constructing a graph from a halo catalog using halo positions and velocity moduli. We then feed the graphs to a GNN and train it to perform parameter inference for Ωm. After training the model, we use symbolic regression to extract the equations from each component of the GNN architecture. Finally, we assemble the equations into one expression and use it to predict Ωm from halos and galaxies of various N-body and hydrodynamic simulations.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Typical pointing corrections for the 40 GHz array. Corrections in azimuth, elevation, and boresight angle are shown in blue, orange, and green, respectively. Left: corrections as a function of azimuth at an elevation of 45◦ and a boresight angle of 0◦. Middle: corrections as a function of elevation at an azimuth of 180◦ and a boresight angle of 0◦. Right: corrections as a function of boresight angle at an azimuth of 180◦ and an elevation of 45◦.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Overview of the galaxy samples. The galaxy pair (#110 and #111) are labeled as triangles with cyan edge. (a) The spatial distribution of galaxies, color-coded by radial velocities Δv relative to the group center. The observation fields of FAST (dashed–dotted green line) and WALLABY (dashed purple line) are drawn. Two dotted gray circles of radii one and two times R 200 indicate the range of N4636G. (b) The spatial distribution of H I detections (blue diamonds) and nondetections (orange circles). Galaxies without SFR measurements are overlaid with gray crosses, and those with only lower-limit estimations of SFR are edged with salmon pink. (c) Galaxies plotted on projected PSD, color-coded by their deviations from the mean M H I  relation of local late-type galaxies (LTGs; see Figure 3). The abscissa is the projected distance d proj from the center of N4636G normalized by R 200; the ordinate is ∣Δv∣ normalized by N4636G’s 1D velocity dispersion σ  v . H I nondetections (light-gray edged circles) are color-coded according to their upper limits of M H I  (see Section 4). The projected escape velocity v esc,proj profile and the virialized region are plotted as dotted gray lines. (d) Projected PSD color-coded by deviations from the star-forming main sequence (SFMS; see Figure 3). H I detections and nondetections without SFR measurements are represented as bold and regular salmon crosses, respectively. Salmon-edged diamonds are galaxies with only lower limits of SFR.
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: The radial metallicity distributions of member stars of H1 and H2. Red, blue, and black colors represent H1, H2, and the disk sample, respectively. (a) The small dots in the background are the member stars, while star symbols represent median values of R and [Fe/H] in each radial bin. The 10 radial bins with the same number of stars are used. Three straight lines and stripes are linear fits of star symbols and their 1σ uncertainties, respectively. (b) We show normalized count density distributions of H1, H2, and the disk sample as functions of [Fe/H]. Three vertical lines show the median metallicity position of each sample. (c) We show the residuals of [H1 − disk] and [H2 − disk].
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: The V  R  vs. V  ϕ  distributions of stars in spatial bins. Each subplot represents a spatial bin, as annotated by the subtitle on the top of each subplot. Within each spatial bin, the wavelet transformation is applied to reveal density distributions of stars in the V  R –V  ϕ  coordinate, as shown by the contours. The background 2D histogram shows direct grid distributions of stars, and the darker grayscale indicates higher star counts in the velocity bin. The shaded regions show the selected positions of H1 (relatively darker) and H2 (lighter) according to the wavelet contours.
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: The metallicity gradients against V  ϕ  distributions of member stars of H1 and H2 in radial bins. Red, blue, and black colors represent H1, H2, and the disk sample, respectively. The star symbols represent the slopes of fitted straight lines for [Fe/H] vs. V  ϕ  in corresponding radial bins. Three horizontal lines and stripes respectively show the mean values and the 1σ uncertainty of the mean value.
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: The same as Figure 2 but for age. This figure shows radial age distributions of the member stars of H1 and H2. Red, blue, and black colors represent H1, H2, and the disk sample, respectively. In the left two panels (a) and (d), the background small dots are the member stars, while star symbols represent the median values of R and age in each radial bin. The five radial bins with the same number of stars are used. Three straight lines and shaded stripes are linear fits of star symbols and their 1σ uncertainties, respectively. Similarly to metallicity distribution, we also show normalized count density distributions and the residuals for age distributions in the right panels (b), (c), (e), and (f).
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: Velocity distributions of stars in spatial bins. These subplots are similar to those in Figure 1 but for all spatial bins. The layout of subplots shows the spatial distribution of bins.
Paper: Connection between Polytropic Index and Heating
Authors: G. Livadiotis, D. J. McComas
Figure caption: Spectrum-like arrangement of polytropic processes. The polytropic index γ (involved in P ∝ n  γ ), the relevant exponent ν ≡ 1/(γ − 1) (involved in n ∝ T  ν ), and the corresponding relations between pressure P, temperature T, and density n, are indicated (taken from Livadiotis & McComas 2012; see also Figure 1 in Livadiotis 2016).
Paper: Connection between Polytropic Index and Heating
Authors: G. Livadiotis, D. J. McComas
Figure caption: Solar wind plasma expands into the heliosphere under polytropic processes. The plot of temperature profile uses the approximation of constant polytropic index γ and density exponent a  n , following Equation (15). If there were no heating, the plasma would expand under simple adiabatic cooling. However, the presence of heating results in a lower polytropic index and higher temperature.
Paper: On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao, Zhaoyu Li, Jiajun Zhang, Yaqian Wu
Figure caption: The age gradients against V  ϕ  of the member stars of H1 and H2. Red, blue, and black colors represent H1, H2, and the disk sample, respectively. The star symbols represent the slopes of fitted straight lines for age vs. V  ϕ  in corresponding radial bins. Three horizontal lines and shaded stripes respectively show the mean values and the 1σ uncertainties.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Following rows from top to bottom and panels from left to right, this figure presents the H2S(33,0–32,1), HC3N(33–32), H2CO(41,3–31,2), CH3OH(31,2–20,2), SO2(126,6–135,9), and SO2(92,8–81,7) moment 0 images. Contours represent the continuum emission at 3, 15, and 100 times the rms noise level of 140 μJy beam−1. Synthesized beams appear in the bottom right corner.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Radial behavior of the excitation temperature, column density, and offset radial velocity from the hot molecular disk component (black symbols) and the warm envelope component (red symbols). The spatial offsets are estimated assuming a disk/envelope model with a position angle of 113° and an inclination of 49° (0° for a face-on disk). The hot compact disk extends up to R ≃ 360 au. T ex ∝ T 0/R (dotted curves for different values of T 0). ﹩{N}_{\mathrm{CH}3\mathrm{CN}}=(500\cdot {X}_{\mathrm{CH}3\mathrm{CN}}/({\mu }_{{mH}}))\cdot \sqrt{100\,\mathrm{au}/R}﹩ (dotted curves for various abundances ﹩{X}_{\mathrm{CH}3\mathrm{CN}}﹩). V off velocity relative to the systemic velocity (12.1 km s−1) vs. deprojected spatial offsets (the system inclination is taken into account). The dotted lines show the Keplerian rotation curves for different central masses. Offset error bars are 50 au, ∼1/4 of the beam size.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: ALMA 0.98 mm dust continuum emission toward GGD 27-MM1. Contours display the emission at levels 5, 10, 15, 25, 75, and 375 times the rms noise level of the image, ∼0.14 mJy beam−1. The synthesized beam is shown in the bottom right.
Paper: Connection between Polytropic Index and Heating
Authors: G. Livadiotis, D. J. McComas
Figure caption: Radial profile of the (a) heat gradient and (b) polytropic index in the inner heliosphere. (a) The heating model Equation 47a includes two terms: (i) a solar-origin term, caused by large-scale energy fluctuations, and (ii) a interstellar PUI term, caused by the excitation of plasma waves by newborn interstellar pickup ions. (b) The polytropic model is derived by substituting the heating model in (a) into Equation (44) leading to Equation 47(c).
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: CH3CN maps obtained from the fit to the compact hot molecular disk (upper panels), and the warm envelope (bottom panels). From left to right are the column density, ﹩{{N}}_{\mathrm{CH}3\mathrm{CN}}﹩, in units per square centimeter, the excitation temperature, T ex, in units of K, and the LSR velocity, V rad, in units of kilometers per second.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Number of velocity components found in the spectra of the CH3CN (17–16) ladder emission toward GGD 27-MM1. Contours show the integrated intensity from CH3CN K = 3. Pixel size roughly coincides with the beam size.