adsabs/AstroCLIMB huggingface dataset:
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Corner plot showing the posteriors and retrieved best-fit parameters for our best chemically consistent fit, labeled “Disequilibrium, No Na, K, Clear” in Tables 6 and 7 and in Figure 13.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Corner plot showing the posteriors and retrieved best-fit parameters for our best free chemistry fit, labeled “H2O” in Tables 6 and 7 and in Figure 13.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: The difference between the predicted t 0, found using the t 0 and P from Table 5, and the fit t 0 for both the photometric transits used in Section 3.1 (blue) and our own Magellan transits (red) as given in Table 5. We see no evidence for transit-timing variations in these data.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Same as Figure 3, but for T2. Note the appearance of bin 12 (7160−7310 Å), which shows strange behavior and is left out of the final analysis.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Same as Figure 3, but for T2.2. Note that this only covers the bluest 11 wavelength bins, as shown in Table 4.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Same as Figure 3, but for T4.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Same as Figure 3, but for T1.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Same as Figure 3, but for T3.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: The best-fit retrieval for our data, the Disequilibrium, No Na, K, Clear case, plotted with the transmission spectrum. Shown in the zoomed-in box in the lower left are 1000 samples of our retrieval. The retrieval is extended down to 0.3 μm and out to 5 μm to show features in the UV and near-IR, which are observable with HST and JWST.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Left: simulated observations of HATS-5b with JWST NIRSpec PRISM based on our best-fit Disequilibrium, No Na, K, Clear model, shown with the Magellan/IMACS results from this paper. Note that the red open circles correspond to binned JWST data, shown for visualization purposes, but that all fitting was carried out for the unbinned data. We label features of interest as well. Right: the change in our posteriors between the Disequilibrium, No Na, K, Clear retrieval (the underlying model fed into the JWST simulations) and the new JWST retrieval, which illustrates the significant improvement in our determination of atmospheric parameters.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Results from our joint fit to all available HATS-5b photometry from HAT-South, TESS (top panels), and GROND (middle panels), along with RVs from Subaru and PFS (bottom panel). Blue bands denote the 68% credibility bands of our photometric models and the 68%, 95%, and 99% credibility bands for the RV. Note that for the photometric data the open circles correspond to binned data, shown for visualization purposes, but that all fitting was carried out for the unbinned data.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: An example result (T5) of our wavelength-dependent curve detrending and fitting. Left: raw target magnitude with corresponding GP systematics model, shown with 68% and 95% errors. Middle: detrended light curve in relative flux, with transit model. Each wavelength bin is labeled with their wavelength range as well. Right: residuals with corresponding standard deviation in ppm. The rest of the wavelength-dependent light curves are given in Appendix B.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: The final averaged transmission spectrum of HATS-5b, obtained as a weighted average of the single transit’s contributions, which are also shown in the top panel. The red and green shaded regions mark the bins where Na I and K I features would be present, respectively.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: The results of our white-light light-curve detrending and fitting, for each of our six transits. Top: raw target magnitude with corresponding GP systematics model, shown with 68% and 95% errors. Middle: detrended light-curve in relative flux, with transit model. Bottom: residuals with corresponding standard deviation in ppm.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: Corner plot showing the posterior distributions for the parameters shown in Table 5 for all of the transits.
Paper: The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at ≈2 au
Authors: Yunlin Zeng, Timothy D. Brandt, Gongjie Li, Trent J. Dupuy, Yiting Li, G. Mirek Brandt, Jay Farihi, Jonathan Horner, Robert A. Wittenmyer, R. Paul. Butler, Christopher G. Tinney, Bradley D. Carter, Duncan J. Wright, Hugh R. A. Jones, Simon J. O'Toole
Figure caption: Total mass of the protoplanetary disk of Gl 86 A in terms of Reynolds number and accretion rate. The mass is negligible in the lower left corner, with small Reynolds numbers and low accretion rates, and large in the upper right corner, with large Reynolds numbers and large accretion rates. The dashed white line indicates a disk mass of 1000  M ⊕, or 3.0 × 10−3  M ☉, or a dust mass of 10 M ⊕ assuming a dust-to-gas ratio of 10−2. The dashed–dotted white line represents 5 M Jup disk mass. The protoplanetary disk of Gl 86 A must have occupied the space to the right of these white lines in order to have possibly formed Gl 86 Ab. To the right of the pink line the disk is Toomre unstable (Q < 1) at its truncation radius.
Paper: The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at ≈2 au
Authors: Yunlin Zeng, Timothy D. Brandt, Gongjie Li, Trent J. Dupuy, Yiting Li, G. Mirek Brandt, Jay Farihi, Jonathan Horner, Robert A. Wittenmyer, R. Paul. Butler, Christopher G. Tinney, Bradley D. Carter, Duncan J. Wright, Hugh R. A. Jones, Simon J. O'Toole
Figure caption: Left: locations of resonant interactions between the circumstellar disk around the present Gl 86 A and the primordial orbit of Gl 86 A and B. The present eccentricity is shown by a vertical line, while different colors indicate different Reynolds numbers. Because the Reynolds number is inversely proportional to the viscosity coefficient, a larger Reynolds number means smaller viscous stress. The squares on each strip represent a large enough eccentricity that gives rise to a resonant torque that overcomes the viscous stress. From the plot, we can read off the truncation radii of Gl 86's protoplanetary disk for different Reynolds numbers. Black circles indicate those radii (AL94). Right: the truncation radii in terms of the Reynolds numbers at e = 0.429. The black circles are the truncation radii corresponding to a sequence of Reynolds numbers starting from 103 to 1014, incrementing with a factor of 10 for each step.
Paper: The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at ≈2 au
Authors: Yunlin Zeng, Timothy D. Brandt, Gongjie Li, Trent J. Dupuy, Yiting Li, G. Mirek Brandt, Jay Farihi, Jonathan Horner, Robert A. Wittenmyer, R. Paul. Butler, Christopher G. Tinney, Bradley D. Carter, Duncan J. Wright, Hugh R. A. Jones, Simon J. O'Toole
Figure caption: The secular evolution of the semimajor axis (left) and eccentricity (right) of Gl 86's orbit since the AGB phase of Gl 86 B assuming constant mass loss. The yellow curves are the simulation results from Mercury. The dashed black curves are analytic expectations from theory. The semimajor axis goes from 15.0 to 23.7 au,   and the eccentricity remains unchanged.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: rms deviation plot, as a function of bin size for each observed transit of TOI-674 b. The dotted red line shows the expected ﹩\sqrt{N}﹩ trend for uncorrelated noise, and the black lines show the normalized rms trend.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Observed minus calculated transit times for TOI-674 b across all sectors of TESS data. The transit times do not significantly deviate from a linear ephemeris.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Example JWST Cases: one with solar metallicity and high altitude clouds, and one with high metallicity and a clear atmosphere. Both are consistent with our observed HST WFC3 data, and need the precision that JWST provides to disambiguate the two models and precisely measure the abundances of the marked absorbers.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: The folded TESS transit data, with the fitted light curve. The data has been binned to a 10 minute cadence.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: The individual visit spectra for TOI-674 b, and the weighted average spectrum based on all three HST visits.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: All three sectors of TESS transit data, binned to 20 minutes cadence, with the fitted light curve.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Detrended spectral light curves and the transit models for the first transit of TOI-674 b.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: 3 and 1 sigma intervals for the full model. The solid blue line is the best-fit model from the full retrieval.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: 2D posteriors for the full retrieval model.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: The same as the Figure A3, but for the remaining epochs.
Paper: X-Ray Emission from the Exoplanet Hosting LTT 1445 Triple Star System
Authors: Alexander Brown, Cynthia S. Froning, Allison Youngblood, Kevin France, David J. Wilson, Girish Duvvuri, Yamila Miguel, Hannah Diamond-Lowe
Figure caption: X-ray to bolometric luminosity ratios for the LTT 1445 X-ray sources as a function of Rossby number. Mean X-ray emission for each star is shown as red circles. The different activity levels of LTT 1445A are shown as filled squares: quiescent (Q—orange), elevated (E—green), and flare (F—blue). The nearby M-dwarf sample included in Wright et al. (2018) and Wright et al. (2011) are shown as black asterisks. The empirical relationships between the X-ray to bolometric luminosity ratio and Rossby number (rotation period/convective turnover timescale) derived by Wright et al. (2018, 2011) from larger samples of F-M type dwarfs are plotted as solid and dashed lines, respectively. The M-dwarf saturated activity level of Pizzolato et al. (2003) is shown as a dotted–dashed line.
Paper: X-Ray Emission from the Exoplanet Hosting LTT 1445 Triple Star System
Authors: Alexander Brown, Cynthia S. Froning, Allison Youngblood, Kevin France, David J. Wilson, Girish Duvvuri, Yamila Miguel, Hannah Diamond-Lowe
Figure caption: The Chandra ACIS-S3 light curves for the LTT 14445 X-ray sources. Upper panel: the light curve for LTT 1445A with different activity level segments separated by vertical dashed lines. Two different binning intervals (1.2 ks (20 minutes) and 1.8 ks (30 minutes) are plotted to better track the variability during the flare outburst. Lower panel: the combined signal from the BC binary with 900 sec binning (filled dots), and the signal from the B component alone extracted using a small 1.″0 radius circular region and then scaled to recover the likely full PSF signal (open squares). For the BC source the largest flare was also measured separately.
Paper: X-Ray Emission from the Exoplanet Hosting LTT 1445 Triple Star System
Authors: Alexander Brown, Cynthia S. Froning, Allison Youngblood, Kevin France, David J. Wilson, Girish Duvvuri, Yamila Miguel, Hannah Diamond-Lowe
Figure caption: Examples of XSPEC spectral fitting to Chandra CCD-resolution spectra. These figures demonstrate the fitting framework within XSPEC. The spectral data with associated error bars are overlaid on the final model shown as a histogram. Right panel: a one-temperature (1-T) fit to the flare spectrum of LTT 1445A grouped with 17 events per channel. Left panel: a two-temperature (2-T) fit to the flare spectrum of LTT 1445 CB grouped with 40 events per channel.
Paper: X-Ray Emission from the Exoplanet Hosting LTT 1445 Triple Star System
Authors: Alexander Brown, Cynthia S. Froning, Allison Youngblood, Kevin France, David J. Wilson, Girish Duvvuri, Yamila Miguel, Hannah Diamond-Lowe
Figure caption: The reconstructed Chandra ACIS-S3 image of LTT 1445. North is up and east to the left. The coordinate grid spacing is 5″ in decl. and 0.5 s of time in R.A. The color wedge illustrates the integrated number of counts per 0.″5 pixel. LTT 1445A is the fainter source at the center of the image with the brighter resolved BC binary to the NW.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: A model of the envelope around the supergiant VY CMa. The central supergiant star is surrounded by a thick dusty cocoon with openning holes. Light from the central supergiant star can only escape through the opennings and is scattered by dusty blobs in the outflow toward the observer, resulting in the large linear polarization observed in the optical spectrum. Absorption by atomic and molecular species within the dusty clumps or blobs produces the observed depolarization with respect to the adjacent continuum.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Spectropolarimetric spectrum of Hα and Ca I] lines in VY CMa.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Spectrum of TiO γ bands in VY CMa and the corresponding Q and U Stokes parameters.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Spectrum of K I doublet and the corresponding Q and U Stokes parameters.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Plot in the (Q, U) plane of Ca I] semiforbidden line.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Simulated emission of TiO γ′ bands from VY CMa shown in solid line. Stokes parameter Q, scaled and shifted for clarity, is also shown in dotted line for comparison.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: Plot in the (Q, U) plane of the absorption lines identified in Figure 10.