adsabs/AstroCLIMB huggingface dataset:
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Clean subtraction rate of galaxies measured from the DECam test. The solid curves show a clean subtraction rate as a function of galaxy magnitude for SFFT (blue) and HOTPANTS (red), with a magnitude bin width of 0.4 mag. The panel insets show examples of the performance of the subtraction for a bright galaxy. The first two panels of the insert show the zoomed-in region around the galaxy from the reference image DECam-SREF and the science image DECam-OBS18a, respectively. The last two panels give the resulting difference image by SFFT and HOTPANTS. The yellow dashed circle indicates the search region for subtraction-induced artifacts with a radius of 11 pixels. The example represents typical cases when SFFT is able to provide a clean subtraction but HOTPANTS failed.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Photometric accuracy measured from light curves of field stars for DECam test. The light curve of each field star (classified as PSF in the Legacy survey) is derived by force aperture photometry on the queue of the convolved images (aliased with the initial DECam-OBS). The force photometry is carried out by SEXTRACTOR with Gaussian optimal aperture 1.3462 × FWHMPTAR, where FWHMPTAR is the FWHM of the specific CCD tile of DECam-PTAR. The photometric uncertainty against star magnitude is shown as blue dots (for SFFT) and red dots (for HOTPANTS). The solid curves denote the median level of the rms in each magnitude bin with a width of 0.2 mag for SFFT (yellow) and HOTPANTS (cyan), respectively.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Computing time on preprocessing vs. the image size of the input data for different methods. The curves with different colors represent the measured time spent on pre-subtraction procedures using different methods on server I (left) and server II (right). Note that each test using SFFT, HOTPANTS, or PyTorchDIA has been repeated with a specified kernel size in each run. Given that the kernel size is irrelevant to preprocessing, we simply use the average time in the figure.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Computing time on image subtraction vs. the image size of input data for different methods. The curves with different colors represent the measured time spent on subtraction using different methods on server I (left) and server II (right). For SFFT, HOTPANTS, and PyTorchDIA, the data points in the curves represent the average time measured from the multiple runs, and the shaded areas indicate the corresponding 1σ standard deviation.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Performance of the image subtraction test using the TMTS images. The figure, from left to right, shows the input reference image TMTS−REF, science image TMTS−SCI, and the resulting difference images by SFFT and HOTPANTS.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: Two ESSW events identified on days 334–339 and days 343–350 in 2009. The panels from top to bottom are (a) V sw (km s−1), (b) N sw (cm−3), (c) carbon and oxygen ion charge state ratios in the same panel, (d) T sw (K), (e) IMF B 0 (nT), (f) B x/B y (nT), (g) B z (nT), (h) B z-V z correlation coefficient, (i) Dst (nT), and (j) AE (nT). The red horizontal line in panel (a) corresponds to V sw = 300 km s−1. The two ESSW events are indicated by vertical shadings. Blue vertical lines indicate HCS crossings.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: Two ESSW events found on days 351–352 and days 360–362 in 2009. The panels from top to bottom are (a) V sw (km s−1), (b) N sw (cm−3), (c) T sw (K), (d) IMF B 0 (nT), (e) B x/B y (nT), (f) B z (nT), (g) B z-V z correlation coefficient, (h) Dst (nT), and (i) AE (nT). The two ESSW events are indicated by vertical shadings. Ion charge state ratios were unavailable for this interval.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: At the top is a schematic of two high-velocity (HSSW) streams and adjacent low-velocity (SSW) streams shown at one instant in time for a steady-state case. The dotted lines represent ideal spiral magnetic field lines and are also the flow lines for the steady-state flow in the corotating frame. The bottom curves show the changes in solar wind parameters as a function of time that will be observed by a spacecraft as the streaming pattern sweeps past. The top curve is V sw, next is the ion density N sw, then the magnetic field magnitude B 0 and at the bottom is the solar wind azimuthal velocity V  φ . S, S’, F, and F’ correspond to SSW, compressed SSW, HSSW, and compressed HSSW, respectively. The locations of the ESSW and the compressed ESSW (ESSW’) are indicated in the top panel by the two blue shaded regions. This figure has been adapted from Belcher & Davis (1971).
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: Distributions of solar wind and geomagnetic activity parameters for the V sw < 300 km s−1 (ESSW) intervals (in red) and for all solar winds with V sw < 300 and ≥ 300 km s−1 (in black) for the entire study interval for panels (b)–(g). In panel (a) the all interval is both the red and black areas. The scales for the distributions of the parameters for ESSW events are given on the right. The scales for the distributions of all parameters for the whole interval of the study are given in the left margins.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: One minute average solar wind data for the high-density region ending the first ESSW event shown in Figure 4. The panels are in the same format as in Figure 4. Black vertical dashed lines indicate interplanetary discontinuities (other than HCS crossings).
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: Two intervals of solar wind data and geomagnetic activity during solar minima are shown, the years 2009 and 2020. The panels are, from top to bottom: V sw (km s−1), B 0 (nT), Esw (mV m−1), Dst (nT), and SME (nT). SME data has been used in place of AE because AE data is not available for 2020. The blue and red horizontal lines in the V sw panel indicate V sw = 750 and 300 km s−1, respectively.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: The format is the same as in Figure 5 (except ion charge state ratios were unavailable). One minute average solar wind data are used to study the high-density region that terminates the second ESSW interval shown in Figure 6.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: This plot shows the halo properties measured from the ESDs of our 35 lens samples. Shown in the different columns are the results for the lens samples in different redshift bins, as indicated at the top of each column. The x-axis is the halo mass measured from weak lensing. The data points in each panel show the best-fit values for the BCG centroid schemes. The panels in the top row show comparisons between the lensing halo mass (﹩\mathrm{log}{M}_{{\rm{h}}}﹩) and the group mass estimated using the abundance-matching method (﹩\mathrm{log}{M}_{{\rm{G}}}﹩). Note that the error along the y-axis is the standard error of the group mass of the sample, while the error along the x-axis indicates the 1σ confidence interval of the fitting. The black lines are reference lines where ﹩\mathrm{log}{M}_{{\rm{G}}}=\mathrm{log}{M}_{{\rm{h}}}﹩. The panels in the middle row show the concentration–mass relation measured from the ESDs. The y-axis is the halo concentration. The theoretical predictions of the c–M relations from Zhao et al. (2009), Dutton & Macció (2014), and Diemer & Joyce (2019) are shown as the solid, dashed, and dashed–dotted lines, respectively. The panels in the bottom row show the halo bias–mass relations. The theoretical predictions of the b–M relations from Jing et al. (1998), Sheth et al. (2001), Seljak & Warren (2004), and Tinker et al. (2010) are shown as the solid, dashed, dashed–dotted, and dotted lines, respectively.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: The distribution of the group/cluster sample in the redshift and mass proxy space. The x-axis is the redshift and the y-axis is the group mass. The black solid lines label the thresholds of our redshift and mass bins. The numbers in each block are the numbers of groups. The top and right panels show the number distributions of the groups using 1D shaded histograms, according to the redshift and group mass, respectively. In the top panel, we also provide the number distributions of the groups after the completeness correction (see Equation (14)), using a red histogram, and the theoretical prediction of the number distribution of halos with mass larger than 1013 h −1 M ⊙ under Planck18 cosmology using a black line (Tinker et al. 2008).
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: An example of the marginalized posterior distributions of the five parameters ﹩\mathrm{log}{M}_{{\rm{h}}}﹩, R sig, f cen, c, and b h for the lens sample with mass ﹩14.0\leqslant \mathrm{log}{M}_{{\rm{G}}}\lt 14.4﹩ at redshift 0.3 ≤ z < 0.4. Here, the red, orange, and green contours show the results for BCG, LWC, and NWC centroids, respectively. The solid red lines show the best-fit results for the BCG sample. The dashed red lines show the 1σ confidence intervals.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: The ESD of the DESI Legacy Imaging Surveys DR9 lens samples in different redshift and mass bins, as indicated, in different columns and rows. In each panel, we compare the results for three different group center indicators. The red points represent the results for the BCG group center, orange those for the LWC, and green those for the NWC. We can see that the BCG performs best as a center indicator. The solid line in each panel shows the best-fit model (Equation (7)) of the ESD for the BCG centroid. The dark and light gray shaded regions represent the 68% and 95% confidence regions of the ESD fitting results, respectively.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: The best-fit results and different model components for a lens sample with mass ﹩14.0\leqslant \mathrm{log}{M}_{{\rm{G}}}\lt 14.4﹩ at redshift 0.3 ≤ z < 0.4. The dark and light gray shaded regions represent the 68% and 95% confidence intervals of the total ESD fitting results, respectively. The three panels correspond to the three different types of group center. The different colored lines represent the halo components labeled in the legend. The χ 2/ν value is also provided in each panel. Note that the degrees of freedom have a value of ν = 15 here.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: The CHMFs in five different redshift bins. The red points with error bars show the CHMFs obtained from the weak-lensing ESD measurements. The black dashed lines show the CHMFs obtained from the group catalog of Y21, with a correction using Equation (14). The black solid lines show the theoretical CHMFs using fitting functions from Tinker et al. (2008) under the Planck18 cosmology.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: We compare our concentration and bias measurements to previous observations by I22 and S22, using different types of symbols, with average redshift of each sample within 0.2 ≤ z < 0.6. Here, we only show the results in three redshift bins, within 0.2 ≤ z < 0.5. We present the theoretical predictions under the Planck18 cosmology with the solid lines and the prediction under the cosmology obtained in I22 with the dashed lines.
Paper: Halo Properties and Mass Functions of Groups/Clusters from the DESI Legacy Imaging Surveys DR9
Authors: Jiaqi Wang, Xiaohu Yang, Jun Zhang, Hekun Li, Matthew Fong, Haojie Xu, Min He, Yizhou Gu, Wentao Luo, Fuyu Dong, Yirong Wang, Qingyang Li, Antonios Katsianis, Haoran Wang, Zhi Shen, Pedro Alonso Vaquero, Cong Liu, Yiqi Huang, Zhenjie Liu
Figure caption: Similar to Figure 5, but here for the three centroids separately. The red, orange, and green points in each panel show the results obtained from signals using the BCG, LWC, and NWC as the center indicators, respectively.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Trajectories of (324) Bamberga through RA13HDEC-25 (top panel) and (13) Egeria and (22) Kalliope through RA23HDEC-25 (bottom panel). The shaded gray regions represent the field boundaries. The dotted and dashed lines represent the asteroids’ long-term trajectories, which trace out loops due to parallax motion. Each colored dot represents the asteroids’ positions at the time of an observation of the field. The size of each dot represents flux density at 2.0 mm predicted by the NEATM. The stars and arrows point toward the mean locations of the Sun during the observation periods.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Light curves of (324) Bamberga (top panel), (13) Egeria (middle panel), and (22) Kalliope (bottom panel) at 2.0 mm. The dashed red lines represent NEATM predictions for flux density. (324) Bamberga is the only asteroid for which we detect statistically significant variation in the light curve of the form predicted by the NEATM.
Paper: Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Authors: P. M. Chichura, A. Foster, C. Patel, N. Ossa-Jaen, P. A. R. Ade, Z. Ahmed, A. J. Anderson, M. Archipley, J. E. Austermann, J. S. Avva, L. Balkenhol, P. S. Barry, R. Basu Thakur, J. A. Beall, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. C. Chiang, H.-M. Cho, T-L. Chou, R. Citron, J.-F. Cliche, T. M. Crawford, A. T. Crites, A. Cukierman, C. M. Daley, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, D. Dutcher, W. Everett, C. Feng, K. R. Ferguson, J. Fu, S. Galli, J. Gallicchio, A. E. Gambrel, R. W. Gardner, E. M. George, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, T. de Haan, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C.-L. Kuo, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, C. Lu, D. P. Marrone, J. J. McMahon, S. S. Meyer, D. Michalik, M. Millea, L. M. Mocanu, J. Montgomery, C. Corbett Moran, A. Nadolski, T. Natoli, H. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, S. Patil, J. Pearson, K. A. Phadke, C. M. Posada, K. Prabhu, C. Pryke, W. Quan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, E. Schiappucci, E. Shirokoff, C. Sievers, G. Smecher, J. A. Sobrin, A. Springmann, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, C. Tandoi, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
Figure caption: Mean flux measurements of (324) Bamberga (top horizontal panels), (13) Egeria (middle horizontal panels), and (22) Kalliope (bottom horizontal panels) at 3.2 mm (left vertical panels) and 2.0 mm (right vertical panels). Color scales for (13) Egeria and (22) Kalliope at 3.2 mm are set at 4σ levels; the rest peak near the mean flux values detected for each asteroid.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Physical structures of the adopted disk models with shadow structures beyond the water snowline. (Left panel): the radial profiles of the gas surface density Σgas(r) [g cm−2] (orange dashed–double-dotted line) and the dust surface density Σdust(r) [g cm−2]. (Right panel): the radial profiles of the gas number density n gas(r) [cm−3] (orange dashed–double-dotted line) and the temperature T(r) [K] in the disk midplane. In the profiles of Σdust(r) and T(r), the black solid lines, the red dashed lines, the blue dotted lines, and the green dashed–dotted lines show the profiles for different values of the parameter f (= 1.0, 0.3, 0.03, and 0.003), respectively.