adsabs/AstroCLIMB huggingface dataset:
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Collage of selected serendipitous archival observations of C/2019 E3, displayed in logarithmic scale at preperihelion heliocentric distances from ∼23 to 13 au. The comet is placed at the center of each panel. White stripes in some of the panels are CCD chip/cell gaps. Position angles of the antisolar direction and the negative heliocentric velocity projected in the sky plane are marked by the red and yellow arrows, respectively. Also shown are two scale bars, one with apparent lengths labeled, and the other one in magenta representing a linear length of 105 km projected at the observer-centric distance of the comet. J2000 equatorial north points upward and east to the left.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Apparent magnitude of comet C/2019 E3 in multiple bands in the SDSS system measured with a 3 × 104 km radius aperture vs. time. Data points are color coded according to the calibrated photometric bands and plotted in different symbols representing different facilities as shown in the legends. In general, the apparent brightness of the comet increased steadily as it approached perihelion.
Paper: Serendipitous Archival Observations of a New Ultradistant Comet C/2019 E3 (ATLAS)
Authors: Man-To Hui, 文韜 許, Robert Weryk, Marco Micheli, Zhong Huang, 中 黃, Richard Wainscoat
Figure caption: Normalized radial surface brightness profiles of C/2019 E3 from (a) 2019 April 5 in the PS1 data and (b) 2019 June 8 in the DECam data. Azimuthally mean values are plotted in olive, with the best-fit power-law radial profiles plotted as pink dashed lines. In each panel, the inner and outer radii of the fitted annular region are marked by two vertical blue lines, and the value of the best-fit logarithmic surface brightness slope is given in the lower left corner.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: The posterior distribution of mass partitioning values for the Kepler-323 system, based on 5000 draws from the posteriors of the planet masses. The solid black line represents the calculated mass partitioning from the maximum likelihood mass probabilities. The three dotted lines represent the mass partitioning value in hypothetical scenarios where one (orange), two (gold), or three (brown) planets of zero mass are also present in the system. The green dashed line represents another hypothetical scenario, where there is a third planet with a mass of 5.5 M ⊕, which minimizes the mass partitioning value. The peak in the posterior near zero is real.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Individual planet radii against their orbital periods and colored by their gap complexity (Gilbert & Fabrycky 2020) for 649 planets (229 planetary systems). For planets colored gray (353 planets in 161 systems), we cannot provide an estimate for the gap complexity because either the system only has two planets, of which gap complexity is undefined, or the system has a planet missing due to the steps outlined in Appendix A. In addition to our measurements for Kepler-323 and Kepler-104 (squares), LTT 1445 A, TOI-125, Kepler-167, and the inner solar system are highlighted for comparison.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Same as Figure 9, but for Kepler-104
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Potential masses of Kepler-323 b vs. potential masses of Kepler-323 c for 5000 random draws from the posteriors of the individual planets, colored by the mass partitioning (Gilbert & Fabrycky 2020). The yellow dot shows the calculated value from the maximum likelihood values and the black line represents a mass partitioning of exactly zero.
Paper: A Tale of Two Peas in a Pod: The Kepler-323 and Kepler-104 Systems
Authors: C. Alexander Thomas, Lauren M. Weiss, Howard Isaacson, Hilke E. Schlichting, Corey Beard, Casey L. Brinkman, Ashley Chontos, Paul Dalba, Fei Dai, Steven Giacalone, Jack Lubin, Judah Van Zandt, Malena Rice
Figure caption: Same as Figure 7, but for Kepler-104.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: CMD (black points) within 120″ of OGLE-2017-BLG-0448 using the OGLE-III star catalog (Szymański et al. 2011). The red asterisk indicates the centroid of the red giant clump. The blue line indicates the blue boundary of the bulge main-sequence stars (Zhang et al. 2023). The yellow-green points show the HST CMD of Holtzman et al. (1998). The blue dot represents the source position for the 2L1S xallarap “Wide A” model. For other models, the source color is the same and the source brightness depends on particular models (Tables 3 and 4). The brown and magenta dots show the secondary sources for the 1L2S parallax (u 0 < 0) and 2L2S “Close Inner” models.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Daily binned data together with the best-fit models of 2L1S parallax, 2L1S xallarap, 3L1S, and 2L2S. All of the four models can remove the long-term residuals shown in Figure 3.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Caustic geometries of the 3L1S models. The locations of the host star, the planet, and the third body are indicated by cyan, blue, and magenta arrows, respectively.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Source trajectories of the 2L1S xallarap models. The symbols are similar to those in Figure 2. Their parameters are given in Tables 3 and 4. The “Close Outer B” and “Close Outer C” models have almost the same trajectories, but their source radii are different.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Best-fit values of the multicomponent Voigt fit analysis of the interstellar gas kinematics. The panels from left to right show the central velocity, the column density of Si II  and Si IV, and the b parameter of the outflow and inflow components detected. The filled blue circles represent the neutral gas traced by Si II, and the filled orange stars represent the ionized gas traced by Si IV. The open blue circles mark the gas components inflowing toward the target star cluster. M51-YSC1 is the exception target for which we used C IV  instead of Si IV. The targets are sorted by the age of the FUV dominant stellar population.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Outflow velocities plotted against six different stellar properties: age of the young stellar population, mass of the young stellar population, mechanical luminosity of stellar winds, mechanical luminosity of SNe, photon production rate, and total mechanical luminosity from stellar winds and SNe. The blue data points represent the neutral gas, whereas the orange data points represent the ionized gas. Open markers (NGC 1566-YSC2, NGC 4485-YSC2, NGC 1566-YSC1, NGC 7793-YSC2, NGC 1313-YSC2, NGC 4656-YSC1) indicate the targets with an age uncertainty larger than 25%, which gives a sense of which data points are the most uncertain in all the plots. Error bars for the outflow velocities are plotted. τ and p are two parameters of the Kendall statistics performed to assess the presence or lack of correlation (see text).
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Outflow velocities plotted against (from top to bottom) the SFR, the SFR per unit stellar mass, and the SFR per unit area. The data points plotted are taken from three different samples: in blue and orange the CLUES neutral and ionized outflows, respectively, in red the CLASSY galactic outflows (Xu et al. 2022); the open circles represent the data points of Heckman et al. (2015), and the black squares represent the data points of Chisholm et al. (2015). In the top panel we report the least-squares linear regression fit for the black squares, the blue circles, and the red plus signs separately.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Kendall statistics for the correlation of outflow velocities with different stellar properties (age, mass, photon production rate, mechanical energy of stellar winds and SNe, mechanical luminosity, here labeled “power,” of stellar winds and SNe) separated into three contributions: young stellar population, old stellar population, and total stellar population. The blue heat maps show the correlations for the neutral outflowing gas, whereas the red heat maps show the correlations for the ionized outflowing gas. The left panels report the Kendall τ coefficients, while the right panels report the p-values with the reversed color bar, so that small values, meaning more significant correlations, appear darker.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Linear regression of the CLUES outflow velocities plotted against SFR per unit area. The blue and orange stars mark the neutral and ionized outflows, respectively, the green line is the best linear fit, and the light-green shaded area is the 95% confidence interval. The dotted and dashed lines are two different feedback models: energy driven and momentum driven, respectively.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Left: kinematics of M95-YSC1 as an example of a target with detected outflow. The absorption profiles in the normalized spectrum for Si II 1526 (dark-blue line) and Si IV 1402 (dark-red line) are plotted on a common velocity axis, tracing neutral and ionized gas, respectively. The light-blue and orange solid lines show the best-fit model, and the dashed color lines show the individual Voigt components of the best-fit model. A vertical black dashed line marks the zero velocity of the gas. Right: same as the left panel, but for NGC 4656-YSC1, an example of a target with a detected inflow.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Outflow velocity plotted against the distance of the CLUES cluster to the center of their host galaxy in units of half-mass radii (Leroy et al. 2021). The data points are color-coded as in Figure 6 according to the phase of the gas: neutral gas in blue and ionized gas in orange. Only the spiral galaxies are included in this figure.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Comparison between stellar feedback and outflow mechanical energy and mechanical power. Only the clusters with an age error smaller than 25% are shown. The markers are color-coded by the age of the cluster (young stellar population), expressed in Myr on the color bar. The solid line, dashed line, and dotted line show the 1:1, 1:10, and 1:100 relations, respectively. For the data points with no error bars, the uncertainties could not be determined realistically owing to numerical precision issues.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Kinematics of neutral and ionized gas surrounding the CLUES clusters. See caption of Figure 8 (continuation).
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: A comparison of the radial column density profiles in HD 100546 (at 50 K) and the radial column densities of the two Herbig Ae disks—HD 163296 and MWC 480—observed in the ALMA large program MAPS (Öberg et al. 2021; Aikawa et al. 2021; Guzmán et al. 2021; Le Gal et al. 2021; Zhang et al. 2021).
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Azimuthally averaged radial emission profiles for the HD 100546 disk generated from the maps presented in Figure 2. The dashed vertical lines mark the locations of peak intensity for the dust rings. The units of the y-axis are mJy beam−1 km s−1 for the molecular lines and mJy beam−1 for the continuum, which is shown on log scale. The horizontal bars show the semimajor axis of the beam for each tracer.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Integrated intensity maps of the 0.9 mm dust continuum emission and molecular line emission from the HD 100546 disk. The continuum map is shown on a log color scale to highlight the weak outer ring of millimeter emission. The beam is shown in the left-hand corner of each panel.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Integrated intensity maps of molecular line emission from the HD 100546 disk with three ellipses overlaid showing the expected morphology of a ring of emission emitting from different heights (Z/R) in the disk. A Z/R = 0 is effectively flat, i.e., emitting from the midplane, and Z/R = 0.25 is the most elevated and this is the measured surface for the 12CO at ≈200 au from both Law et al. (2022) and Stapper et al. (2023).
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: A gallery of sulfur-bearing molecules detected in the HD 100546 disk alongside the 0.9 mm dust emission from Pineda et al. (2019). The location of the putative planet from Currie et al. (2015) and the excess rovibrational CO emission attributed to a forming planet by Brittain et al. (2019) from 2017 are highlighted with a green circle. This is the same region of the disk where the SO emission is peaking. The units of the color bar are mJy beam−1 km s−1 for the molecular lines and mJy beam−1 for the continuum.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Polar deprojection of the HD 100546 integrated intensity maps, which highlight the azimuthal asymmetry in the dust and molecular rings at ≈200 au. The dashed contour traces the 5σ level of the dust continuum emission. The units of the color bar are mJy beam−1 km s−1 for the molecular lines and mJy beam−1 for the continuum.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Color map of the azimuthally averaged dust continuum emission for the HD 100546 disk. The colored markers show the peak location of the different molecular rings where the widths of the horizontal lines show 0.5× the semimajor axis of the beam. Different colors show different elemental/molecular families. The dashed vertical lines mark the location of peak intensity for the dust rings.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Radial column density profiles for the HD 100546 disk determined at a range of assumed excitation temperatures. The C17O profiles break where the optical depth exceeds ≈2.