adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: MAD values corresponding to various extraction widths for Ahsoka order 1 (red) and order 2 (blue). For each extraction width, we computed an MAD value based upon the raw white light curve OOT normalized flux values. We defined the OOT points as those from integration indices 0 through 229, combined with integration indices 600–719. Our final spectral extraction widths (green stars) are those that minimize the MAD in each order. The MAD values for our final extraction widths are labeled next to the green stars on the plot. See text for additional information.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Top panel: contrast curves obtained from Gemini North ’Alopeke and Gemini South Zorro instruments. Insets showcase 832 nm reconstructed images, highlighting the increased contrasts achieved with Zorro on Gemini South due to better seeing conditions and a longer total integration time. No close companion star was detected within the achieved 5σ magnitude contrast curves and angular limits from the 8 m diffraction limit out to 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2. At the distance of TOI-4364, these limits correspond to spatial separations ranging from 0.88 to 52.8 au. Bottom panel: SOAR sensitivity curve taken on 2021 October 18. The 5σ sensitivity limits are shown out to 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩15, corresponding to a projected separation of 138.1 au.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Evolution of the planetary radius as a function of stellar age for TOI-4364b, assuming the best-fit planetary parameters (including planetary mass). The gray and black lines represent the radius evolution predicted by the VPLanet model, which incorporates both planetary cooling and photoevaporation effects. Each line corresponds to a different initial H/He envelope fraction, ranging from 0% to 10%. The red circle marks the observed planetary radius at 710 Myr, with error bars indicating the 1σ uncertainty. The darker contour lines show models that are consistent with the observed radius, which have H/He envelope fractions between 0.4% and 0.9%. The nominal best-fit solution is shown as a thicker line, which corresponds to a current-day envelope fraction of 0.6%. Over time, the planet's radius is expected to decrease gradually owing to continued cooling and mass loss from photoevaporation.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: LCOGT 1 m TOI-4364b follow-up observations (small points) along with binned data (larger circles) and best-fit transit models (black line). Individual observations are shifted along the y-axis for clarity.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: TOI-4364’s distance from the Hyades center over the course of the cluster's lifetime. Each curve shows one simulation with the current position and velocity varied within its uncertainties and traced back through the MWPotential2014 galactic potential (J. Bovy 2015) over the past 700 Myr. The most recent potential pass within the Hyades cluster’s tidal radius was 155 Myr ago, which is a plausible ejection time.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Distance from Earth vs. planet radius for confirmed exoplanets (gray circles), young (<1 Gyr) planets with well-constrained ages (colored circles), previously discovered Hyades exoplanets (pentagons), and TOI-4364b (star). TOI-4364b stands out as a nearby young planet at the upper edge of the radius valley, making it a prime target for atmospheric and evolutionary studies.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Analysis of TOI-4364’s photometric rotation period using TESS Sectors 5 (purple) and 32 (green). Top: trimmed light curve with boxes showing similar structures; middle: PSM output, with maximum likely periods shown with dashed lines; bottom: phase-folded light curves for each sector at P = 10.57 days.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Period–radius distribution of confirmed exoplanets (gray circles), confirmed young (<1 Gyr) exoplanets with well-constrained ages (colored circles), previously discovered Hyades exoplanets (pentagons), and TOI-4364b (star). To enhance the readability of the figure, we omit planets discovered via direct imaging. Note that TOI-4364b resides at the upper edge of the radius valley (blue strip).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: The color−rotation sequence for catalog members of the Hyades cluster, as compared to the Pleiades (120 Myr; L. M. Rebull et al. 2016), Praesepe (670 Myr; S. T. Douglas et al. 2017), and NGC 6811 (1 Gyr; J. L. Curtis et al. 2019). TOI-4364 is depicted as a gold star.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XII. A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster
Authors: Adam Distler, Melinda Soares-Furtado, Andrew Vanderburg, Jack Schulte, Juliette Becker, Andrew W. Mann, Steve B. Howell, Adam L. Kraus, Ronan Kerr, Khalid Barkaoui, César Briceño, Karen A. Collins, Dennis Conti, Jon M. Jenkins, Mary Anne Limbach, Samuel N. Quinn, Richard P. Schwarz, Sara Seager, Jake D. Turner, Joseph D. Twicken, Joshua N. Winn, Carl Ziegler
Figure caption: Top panel: crowding map of TOI-4364 for Sector 5, displaying neighboring sources up to a magnitude difference of Δm = 6. The SPOC aperture is indicated by red squares. Bottom panel: same as the top panel, but for Sector 32.
Paper: The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 
Authors: K. L. Luhman
Figure caption: Left: MK vs. spectral type for members of B209N and the single-star sequence of TWA compared to theoretical isochrones from I. Baraffe et al. (2015; green lines) and the PARSEC models (A. G. Bressan et al. 2012; Y. Chen et al. 2014; magenta lines). The solid lines span masses of 0.2–0.7 M⊙ and the dotted lines extend to 0.1 M⊙ for the Baraffe isochrones. Model temperatures have been converted to spectral types using the temperature scale from G. J. Herczeg & L. A. Hillenbrand (2014). Right: B209N and TWA are compared to the HD 28354 group in Taurus and the single-star sequence of the 32 Ori association shifted to brighter MK by 0.42 mag. Spectral types for TWA and 32 Ori have been derived from GBP–GRP using the relationship between spectral type and GBP–GRP for young stars (K. L. Luhman 2022a).
Paper: The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 
Authors: K. L. Luhman
Figure caption: Equatorial coordinates, extinction-corrected MK vs. spectral type, G vs. parallax, and proper motion offsets for stars that were assigned to the D4-North Taurus population by K21 and that K. L. Luhman (2018, 2022b, 2023a) classified as members of two Taurus groups (B209N, L1495/B209) and two older associations in the vicinity of Taurus (32 Ori, 93 Tau). A fit to the single-star sequence of the Pleiades is indicated in the H–R diagram (red solid line). Error bars are omitted for the distances and proper motion offsets when they are smaller than the symbols.
Paper: The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 
Authors: K. L. Luhman
Figure caption: Equatorial coordinates, extinction-corrected MK vs. spectral type, G vs. parallax, and proper motion offsets for members of the B209N and L1495/B209 groups in Taurus (K. L. Luhman 2023a). The filled triangle in each diagram is IRAS 04125+2902.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 30, but showing the rovibrational band.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 29, but showing the rovibrational band.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 28, but showing the rovibrational band.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 30, but showing longer wavelengths.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 28, but showing longer wavelengths.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Same as Figure 29, but showing longer wavelengths.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Excess absorption as a function of time and wavelength in the stellar frame, for planets b (left) and c (center and right). The top and bottom white lines represent white-light ingress and egress, while the slanted red lines indicate the wavelengths of the helium triplet in the planetary frame. The data behind this figure are available in six ASCII data files. A Python script is provided to read these files and recreate the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Average in-transit excess absorption in the planetary frame for all three visits. The error bars are underestimated because they only include the photon noise, read noise, and flat-fielding error, not systematics. Visits b and c2 are directly comparable because they both include a full transit and baseline on both sides, but c1 is not directly comparable because it is a partial transit. The data behind this figure are available in machine-readable format.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Band-integrated light curves for planets b (left) and c (right). The band we adopt is 10833.27 ± 0.75 Å, covering the main helium peak. The data are binned by a factor of 4 for all visits. The data behind this figure are available in machine-readable format.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Absorption predicted by pyTPCI for planet c, assuming arbitrarily that the outflow has a hard outer cutoff of 5 Rp, and that all the metastable helium disappears at higher radius. This is likely a severe overestimation of the effects of confinement by magnetic fields or stellar winds, because a confined outflow does not disappear and should still absorb in the helium triplet.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: pyTPCI predictions for c (top) and b (bottom) at different metallicities, compared to the observational data. For c, we run one simulation with the XUV spectrum from David Wilson and another with the XUV spectrum from Jorge Sanz-Forcada. Despite the factor of 3–4 flux discrepancy in both X-rays and EUV, the resulting helium absorption is remarkably similar.
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Two different XUV spectrum reconstructions: one by A. Youngblood’s group following the methodology in G. M. Duvvuri et al. (2021, 2023) and one by J. Sanz-Forcada following the methodology in J. Sanz-Forcada et al. (2025).
Paper: Constraining Atmospheric Composition from the Outflow: Helium Observations Reveal the Fundamental Properties of Two Planets Straddling the Radius Gap
Authors: Michael Zhang, Jacob L. Bean, David Wilson, Girish Duvvuri, Christian Schneider, Heather A. Knutson, Fei Dai, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Avi Shporer, Keith Horne, Ramotholo Sefako, Felipe Murgas, Enric Palle
Figure caption: Top: the TTVs of TOI-836 c and the best-fit sinusoidal model to the TTVs. The vertical green lines indicate the times of our two helium visits. Bottom: the residuals of the fit.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Model fits for all disks that met the S/N threshold in each progression. Line profiles are fit with either one or two Gaussian components based on the criteria (e.g., ΔBIC) discussed in the text. The coadded profiles are in blue, and the best-fit models are in red. Single and narrow Gaussian components are marked with orange dashed lines, broad Gaussian components with green dashed lines, and the linear continuum with gray dashed lines. The sum of the broad and narrow Gaussian components exceeds the height of the best-fit model because the best-fit model is convolved with the HST-COS LSF (not shown). Velocities are not corrected for the stellar reference frame.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Cumulative distribution functions of physical parameters for 12CO, 13CO, and C18O clumps, including line width (Δv), effective radius (Reff), mass of clumps (Mclump), virial parameter (αvir), surface density (Σ), and number density (﹩{N}_{{{\rm{H}}}_{2}}﹩). The median values of the physical parameters for the different CO isotopes are denoted by dashed lines and marked in the lower-right corner of each panel.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: The relationship between the mass and the effective radius of the clump. The upper and lower solid black lines represent surface densities of 1 g cm−2 (M. R. Krumholz & C. F. McKee 2008) and 0.05 g cm−2 (J. Kauffmann et al. 2013), respectively. The yellow shaded region shows the region where the mass of the clump is insufficient to form massive stars, and is defined as M(r) ≤ 870 M⊙(r/pc)1.33. The three dashed lines represent the linear fit to the corresponding CO clumps.
Paper: Distributions and Physical Properties of Molecular Clouds in the G24 Region of the Milky Way
Authors: Tian Yang, Xi Chen, Xiao-Yun Xu, Yang Yang, En Chen, Jun Li, Bing-Gang Ju, Deng-Rong Lu
Figure caption: Spatial distribution of the infall candidates identified from the HCO+ line profiles. The background is the integrated intensity map of C18O emission. The ellipses indicate the location of the C18O clumps, where cyan colored ones indicate the locations of the C18O clumps with non-blue HCO+ profiles, while red, green, and blue colored ones indicate the locations of the C18O clumps with double-peak HCO+, peak-shoulder HCO+, and single-peak HCO+ profiles with the peak skewed toward the blue, respectively.