adsabs/AstroCLIMB huggingface dataset:
Paper: SOLES XII. The Aligned Orbit of TOI-2533 b, a Transiting Brown Dwarf Orbiting an F8-type Star
Authors: Thiago Ferreira dos Santos, Malena Rice, Xian-Yu Wang, Songhu Wang
Figure caption: Best-fit joint model for TOI-2533 b. Panel (a) presents the phase-folded TESS light curve, panel (b) the TRES radial velocity observations, and panel (c) the NEID Rossiter–McLaughlin observations. The residuals are presented at the bottom of each panel, along with the 1σ uncertainty of the joint model in gray. A schematic representation of the TOI-2533 b side-view orbit is presented at the bottom left of the panel (c), corresponding to a sky-projected obliquity of λ = −7° ± 14°.
Paper: Surviving in the Hot-Neptune Desert: The Discovery of the Ultrahot Neptune TOI-3261b
Authors: Emma Nabbie, Chelsea X. Huang, Jennifer A. Burt, David J. Armstrong, Eric E. Mamajek, Vardan Adibekyan, Sérgio G. Sousa, Eric D. Lopez, Daniel Thorngren, Jorge Fernández Fernández, Gongjie Li, James S. Jenkins, Jose I. Vines, João Gomes da Silva, Robert A. Wittenmyer, Daniel Bayliss, César Briceño, Karen A. Collins, Xavier Dumusque, Keith Horne, Marcelo Aron F. Keniger, Nicholas Law, Jorge Lillo-Box, Shang-Fei Liu, Andrew W. Mann, Louise D. Nielsen, Ares Osborn, Howard M. Relles, José J. Rodrigues, Juan Serrano Bell, Gregor Srdoc, Chris Stockdale, Paul A. Strøm, Cristilyn N. Watkins, Peter J. Wheatley, Duncan J. Wright, George Zhou, Carl Ziegler, George Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn, Jon M. Jenkins, Michael Fausnaugh, Michelle Kunimoto, Hugh P. Osborn, Samuel N. Quinn, Bill Wohler
Figure caption: Evolution of TOI-3261b’s semimajor axis (top) and mass (bottom) as a result of tidal stripping via Roche Lobe Overflow, following the approach of Gu et al. (2003). The star denotes the planet’s current position and mass.
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Corner plot corresponding to the MCMC fit to the BT-Settl model grid. Marginalized posteriors are shown on the diagonal, with covariance between all parameters in corresponding 2D histograms. Dashed lines show 16th, 50th, and 84th percentile statistical errors. Although this analysis results in small statistical error bars for temperature and ﹩\mathrm{log}(g)﹩, this is not a realistic representation of our constraints on these terms. We instead adopt errors the size of the grid spacing for the rest of the paper as our analysis strongly prefers grid points. Measurements for spin and RV are insensitive to changes of temperature or ﹩\mathrm{log}(g)﹩ as large as the grid spacing; see Section 5.1.
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Best-fit 100 random draw orbits for κ And b, using companion RVs and the HGCA (Brandt 2021) with the orbitize! package. Upper left: ΔR.A. and Δdecl. coordinate best fits for the κ And b system (blue/green lines) and the relative astrometry (red stars) from Bowler et al. (2020). Upper right, top: separation (ρ) in milliarcsecond best fits (gray lines) with relative astrometry (red stars) from Bowler et al. (2020); Upper right, bottom: position angles (PAs) in degree best fits (gray lines) with the relative astrometry (red stars) from Bowler et al. (2020). Middle: RV orbit best fits (gray lines) for the host star κ And A. Bottom: RV orbit best fits (gray lines) for the κ And b using KPIC measurements (blue triangles).
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Spin measurements from low-mass companions and solar system planets, with those from the published KPIC sample marked with a star. κ And b, shown with a pink star, is one of the highest points in this comparison. Other known companions are marked with a green triangle, and known dynamical mass measurements are marked with a blue diamond. Detection limits for ﹩v\sin (i)﹩ (≤5 km s−1) are indicated by blue dashed line. We also include random draws from the Wang et al. (2021) solutions for the best-fit rotational trend, in light blue.
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Posteriors of the best-fit orbital solutions for κ And b using companion RVs, astrometry (Bowler et al. 2020), and the HGCA (Brandt 2021) with the orbitize! package (Blunt et al. 2020).
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Extracted spectra in NIRSPEC orders 31–33 used in the fit compared to the best-fitting forward model for that order, with contributions from companion and speckle flux also shown independently.
Paper:  κ Andromedae b Is a Fast Rotator from KPIC High-resolution Spectroscopy
Authors: Evan C. Morris, Jason J. Wang, 劲飞 王, Chih-Chun Hsu, Jean-Baptiste Ruffio, Jerry W. Xuan, Jacques-Robert Delorme, Callie Hood, Marta L. Bryan, Emily C. Martin, Jacklyn Pezzato, Dimitri Mawet, Andrew Skemer, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Joshua Liberman, Ronald Lopez, Ben Sappey, Tobias Schofield, J. Kent Wallace, Ji Wang, 吉 王
Figure caption: Cross correlations for individual molecular species. Detections of H2O, CO, and expected nondetection of CH4.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: Mass-size diagram of the prestellar cores in Orion. The blue stars represent the known high-mass prestellar core candidates in the galactic plane for comparison (S. Bontemps et al. 2010; K. Wang et al. 2014; T. Nony et al. 2018; A. T. Barnes et al. 2023; T. Nony et al. 2023). The purple and brown diamonds represent the core properties in this paper observed by JCMT (D. Nutter & D. Ward-Thompson 2007) and ACA. The orange, green, and red dots depict the prestellar/starless cores identified by C. J. Salji et al. (2015), V. Könyves et al. (2020), and H. -W. Yi et al. (2018), respectively. The lines illustrate the mass-size scalings of the clumps, following a turbulence-dominated (M ∝ r 2) or gravity-dominated (M ∝ r) density structure (F. Motte et al. 2018a).
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: N2H+ and N2D+ spectra in nine cores. Left: N2H+ spectra. The red horizontal dotted lines represent 10σ limits, and the red vertical lines represent the integrating range. Right: N2D+ spectra. The red horizontal dotted lines represent 3σ limits, and the red vertical lines represent the integrating range.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: H2CO (32,2 − 22,1) spectra in nine cores. The red dotted lines represent 3σ limits.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: ACA 1.06 mm and 1.34 mm continuum images of seven sources shown in color before primary beam correction. The cyan ellipse represents the size of the identified cores convolved with beam. The white contours show continuum emission at levels of [−6, 6, 12, 24, 48]σ, where σ can be found in Table 2. The blue ellipse in the bottom left marks the synthesized beam.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: CO outflow plots for all cores except ORS-4. The grayscale background image shows the ACA Band 6 continuum emission without primary beam correction. The blue ellipse in the bottom left represents the synthesized beam size of the continuum. Green contours indicate the continuum emission at levels of [6, 12, 24, 48]σ. The blue and red contours represent the blueshifted and redshifted CO emission without primary beam correction, respectively. Contour levels vary due to different emission levels.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: Spatial distribution of seven cores in Orion. The background is the 353 GHz opacity retrieved from M. Lombardi et al. (2014). Two small regions that covers our sample are further zoomed in. The green box represents the position of each core.
Paper: Absence of High-mass Prestellar Cores in the Orion Giant Molecular Cloud
Authors: Wenyu Jiao, Ke Wang, Fengwei Xu
Figure caption: CO outflow of ORS-4_P1. The grayscale background image shows the ACA Band 6 continuum emission. The blue ellipse in the bottom left represents the synthesized beam size of the continuum. The green ellipse marks the position of the cores. The blue and red contours show the blueshifted and redshifted CO emission integrated over [−19, 10] km s−1 and [12, 41] km s−1, at levels of [40, 80, 120, 160] K km s−1.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Upper panels: the spectra and distribution of maser spots for H2O, NH3 (9,6), and CH3OH 22–21 transitions detected in the W51e2 region. The meaning of the colorful lines and gray bars in the spectra is similar to that in Figure 2. For maps of maser spots, the gray contours show the 1.3 mm continuum, with the start, step, and end levels to be 0.002, 0.002, and 0.018 Jy  beam−1. Lower panels: the spectra and distribution of maser spots for H2O and NH3 (9,6) transitions detected in the W51e8 region. The gray contours in maps of maser spots show the 1.3  mm continuum, with the start, step, and end levels to be 0.002, 0.001, and 0.018 Jy beam−1. The black dashed box in the lower-left panel marks the H2O maser spots belonging to W51e8.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: The spectra and spots of all the maser transitions detected toward the W51-North subregion in our VLA observation. For transitions of pure masers, the spectra are shown in colorful lines. The spectra of transitions mixed with maser and nonmasing components are shown in black, and their maser components are marked with gray bars. For maps of maser spots, the gray contours show the 1.3 mm continuum, with the start, step, and end levels to be 0.006, 0.012, and 0.023 Jy beam−1.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Upper panel: the SiO J = 5–4 emission toward W51-IRS2 is shown in red and blue, which correspond to the velocity ranges of 67–97 and −17 to 56 km s−1, while the 1.3 mm continuum emission is presented in green. Lower panel: the HC3N J = 24–23 emission toward W51-IRS2 shown in red and blue corresponds to the velocity ranges of 66–90 and 39–52 km s−1. The white dashed circles mark a compact source to the east of W51-North (see Sections 3.1.3 and 4.4.1).
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: The integrated intensity (moment 0) maps of all the nonmasing transitions detected in W51-IRS2. Contour levels in red for the integrated flux density of different transitions are 0.05, 0.1, 0.2, 0.4, 0.6, 0.8, 1.0, and 1.2 Jy beam−1 km s−1, while those in blue are 0.2 and 0.5 times the peak of the integrated flux density for each transition.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Left panel: a picture of the W51A region extracted from Ginsburg et al. (2017). Its background is made of millimeter emission of lines and continuum from ALMA observations: HC3N 24–23 in purple, C18O 2–1 in blue, CH3OH 42–31 in orange, 1.3 mm continuum in green. Right panel: the dots in blue, red, and green represent the overall distributions of the H2O, NH3(9,6), and CH3OH 42–41 masers in W51A, overlaid on the gray K-band continuum background detected in our VLA observation.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: The spectra and spots of all the maser transitions detected in the W51d2 subregion. The maser emissions are shown with colorful lines in the spectra of the H2O and NH3 (9,6) transitions, and marked with gray bars in the spectra of the NH3 (7,5) and (6,3) transitions. The gray contours in maps of maser spots show the 1.3 mm continuum, of which the start, step, and end levels are the same as that in Figure 2.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Upper-left panel: a figure showing the W51-IRS2 regions taken from Ginsburg et al. (2017). The emission shown in green is the NACO K-band continuum (Barbosa et al. 2008; Figuerêdo et al. 2008), and these in blue and red are the blue- and redshifted CO 2-1 emission (Ginsburg et al. 2017). The blue contours are the H77α RRL transition detected in Ginsburg et al. (2016), and the white contours are the ALMA 1.3 mm continuum (Ginsburg et al. 2017). Upper-right panel: a zoomed version of the region toward a red dashed box in the upper-left panel. The background is the ALMA 1.3 mm continuum from the project 2015.1.01596.S. The contour levels in white for our VLA K-band continuum are 0.05, 0.10, 0.15, 0.20, 0.40, 0.60, and 0.80 Jy beam−1. The red solid ellipse denotes the W51d2 subregion. Lower panel: a zoomed version of the region toward a red dashed box in the upper-right panel. The background is the ALMA 1.3 mm continuum, with gray contours marking the most luminous objects in this region. The “+” symbols mark the location of the H2O maser spots. The labels “mrk[number]” are temporary names given by us for studying these objects or subregions that do not even have a name before. Among them, “mrk1”, “mrk2” and “mrk3” are studied in Sections 4.3.1, 4.3.2 and 4.1, respectively.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Panel (a): a replotted figure of the right panel of Figure 1 in Zhang et al. (2023) to show the maser distribution in W51-North. The light-colored circles and dark-colored squares represent the H2O maser spots detected in our VLA observation and that in Imai et al. (2002), respectively. The reference position is R.A. (J2000) = 19h23m40.ˢ047, decl. (J2000) = +14°31﹩{}^{{\prime} }﹩05.″530. The 1.3 mm continuum detected in the archival ALMA data is shown with dark blue contours, with the start, end, and step levels to be 0.0025, 0.0100, and 0.0025 Jy beam−1, respectively. The “A,” “B,” and “C” labels mark the regions that have shown variations, as shown in Figure 5 in Zhang et al. (2023). Panel (b): the spectra of H2O maser transition extracted from W51-IRS2, W51-North, and W51d2 regions detected with the VLA. The red dashed lines at ∼58 km s−1 in panels (b) and (d) mark the strongest velocity component in the W51d2 subregion. Panel (c): the spatial distribution of H2O maser spots in the whole region of W51-IRS2. Panel (d): the spectra of H2O maser transition detected toward W51-IRS2 using TMRT from 2020 January 8 to April 7, which was taken from Zhang et al. (2022).
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Upper-left panel: same as the detection result of the distribution of H2O maser spots in W51e2 in Figure 6, with names of different regions being marked. Upper-right panel: a zoomed map of the distribution of H2O maser spots, corresponding to the region marked with a gray dashed box in the upper-left panel. Lower-left panel: the 1.3 mm continuum, SiO J = 5–4, and HC3N J = 24–23 emissions in the W51e2 region. For orange contours, the start, step, and end levels are 0.06, 0.01, and 0.10 Jy beam−1, respectively. For cyan contours, the start, step, and end levels are 0.10, 0.10, and 0.50 Jy beam−1, respectively. Lower middle panel: a cartoon taken from Li et al. (2013), which is used to indicate the turbulent entrainment origin of protostellar outflows. In this figure, the pwind and penvelope represent the ram pressure of the wind and the envelope. Lower-right panel: a cartoon taken from López-Vázquez et al. (2024), which is used to indicate the multilayer outflows driven by disk winds of source HH 30.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Upper-left panel: the emission of the SiO J = 5–4 transition from the W51e2 region shown in red and blue corresponding to velocity ranges of 78–159 km s−1 and −54–54 km s−1, respectively. Upper-right panel: the emission of the HC3N J = 24–23 transition from the W51e2 region shown in red and blue corresponding to velocity ranges of 70–80 km s−1 and 28–49 km s−1, respectively. Lower-left panel: the emission of the SiO J = 5–4 transition from the W51e8 region shown in red and blue corresponding to velocity ranges of 70–82 km s−1 and 4–56 km s−1, respectively. Lower-right panel: the emission of the HC3N J = 24–23 transition from the W51e8 region shown in red and blue correspond to velocity ranges of 74–84 km s−1 and 29–52 km s−1, respectively. In all these four subfigures, the 1.3 mm continuum is shown in green.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Left panel: a figure taken from Zhang et al. (2023), of which white circles and orange squares represent the H2O maser spots detected in W51-North from our VLA observation and from Imai et al. (2002). The meaning of the colors in the background is the same as that in the upper panel of Figure 5. Middle panel: white circles represent the H2O maser spots detected in W51e2-E from our VLA observation, and the meaning of colors in the background is the same as that in Figure 7. Right panel: white circles filling in gray represent the H2O maser spots detected in W51e8 from our VLA observation, and their size indicates the flux intensity of the H2O maser spots. Since the flux intensities in W51e8 are much lower than that of other sources, they are amplified about 100 times for clear comparison. The meaning of the colors in the background is the same as that in Figure 7. Notably, the source “W51e4” is beyond the range of this subfigure, although we pointed out the relative direction of the location of this source to the “W51e8” subregion.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Left panel: distributions of maser spots of the typical kinds of maser transitions in W51-North, including H2O, NH3 (9,6), and CH3OH 42–41 ones. Right panel: distributions of maser spots for the NH3 (7,7), (7,6), and (8,6) transitions in W51-North, overlaid on that of H2O maser for comparison. The white contours in both panels show the 1.3 mm continuum emission detected from the ALMA archived data.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Left panel: the spectra of NH3 (9,6) maser transition detected toward W51-IRS2 using TMRT from 2020 January 8 to April 7, which was taken from Zhang et al. (2022). Upper-right panel: the spectra of NH3 (9,6) maser transition extracted from W51-IRS2, W51-North, and W51d2 regions detected with the VLA. The red dashed lines at ∼54.2 km s−1 in the left and upper-right panels mark the strongest velocity component in the W51d2 subregion. Lower-right panel: the spatial distribution of H2O maser spots in the whole region of W51-IRS2.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Left panel: distributions of maser spots of the typical kinds of maser transitions in W51e2-E, such as H2O, NH3 (9,6), CH3OH 41 − 41 and 21 − 21 ones; Right panel: distributions of maser spots for H2O and NH3 (9,6) transitions in W51e8.
Paper: Masers and Star Formation Activities in W51A
Authors: Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shi-Min Song, Jun-Ting Liu, Ying Lu
Figure caption: Distributions of maser spots of the typical kinds of maser transitions in the W51d2 subregion, including H2O, NH3 (9,6), (7,5), and (6,3) ones. The label “mrk2” refers to the arc-shaped distribution of H2O maser spots below the Lacy jet (see details in Section 4.3.2).
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: (Left) Lens mass accuracy distribution vs. lens distance accuracy distribution for the sample of the Roman events presented in the text. The various levels of colors and lines indicates the 39%, 86%, 98.9%, and 99.9% density contours from pyLIMASS while the 1d distributions are also presented. The red cross indicates the median uncertainty, in both directions, reported by pyLIMASS. (Right) Distribution of the mass accuracy vs. the maximum magnitude uncertainty between the lens and the source in the F146 band ΔF146.
Paper: Estimating Microlensing Parameters from Observables and Stellar Isochrones with pyLIMASS
Authors: E. Bachelet, M. Hundertmark, S. Calchi Novati
Figure caption: Lens mass vs. lens distance for MOA-2009-266Lb (Muraki et al. 2011). The various levels of colors and lines indicates the 39%, 86%, 98.9%, and 99.9% density contours from pyLIMASS, while the measurement of Muraki et al. (2011) is displayed in red. The contours have been smoothed with a Gaussian kernel for plotting purposes.