adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Attenuation excess due to the 2175 Å bump (A bump; top) and normalized bump strength (B; bottom) in our sample as a function of sSFR. The black line shows the median values of the results obtained from individual pixels, with gray shaded regions indicating 1σ and 2σ scatters of the data points. The stars are the results from the 1Re  stacks of each galaxy, with color codes showing the total stellar mass of the galaxy (from NSA). In the panels from left to right, colored triangles/lines show the results of subsamples of spaxels selected by A  V  (left), b/a (middle), and galactocentric distance (right). In the bottom panels, the bump strengths for the Milky Way and Calzetti dust curves are indicated by red and blue dashed lines, respectively, with a blue circle indicating the average value of the Milky Way (﹩\mathrm{log}(\mathrm{sSFR}/{\mathrm{Gyr}}^{-1})\sim -1.6﹩).
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Slope of the attenuation curve in NUV (A  w 2 /A  w 1 ). The black line shows the median values of the results obtained from individual pixels, with gray shaded regions indicating 1σ and 2σ scatters of the data points. The stars are the results from the 1Re  stacks of each galaxy, with color codes showing the total stellar mass of the galaxy (from NSA). In the panels from left to right, colored triangles/lines show the results of subsamples of spaxels selected by A  V  (left), b/a (middle), and galactocentric distance (right).
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Results of the test of our method on mock spectra. The histograms show the distributions of the difference between the input and the estimated values for five dust parameters (panels from top to bottom): A  V , A  B /A  V , A  w 2 /A  w 1 , A bump, and B. In each row, the first three panels show the results for three S/N ranges (as indicated) as obtained with the BC03 stellar templates, while the fourth panel shows the result with the BPASS stellar templates for the S/N range of 10 < S/N < 30. In each panel, the filled blue histogram shows the result from mock spectra that include Gaussian noise with a standard deviation of σ  Ks  = 0.07 in the Ks band and σ UV = 0.13 in the uvw2, uvm2, and uvw1 bands, with the mean and standard deviation of the distribution indicated in the top left corner. Red histograms in the first two rows are the results obtained by assuming a smaller uncertainty in the Ks band with σ  Ks  = 0.02, while the orange and red histograms in the third through fifth rows show the results obtained with smaller uncertainties in the NUV bands, with σ UV = 0.05 (orange) and 0.02 (red). All histograms are normalized to have a total of unity. Overall, the tests results show that our method adequately recovers the input properties of dust attenuation with systematic and statistical errors well under control.
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Illustration of the method used in this work. The blue line in the middle panel is one spectrum stacked within 1Re  of our sample galaxy. In the figure, we normalize the spectrum at 5500 Å. We use the method of Li et al. (2020) to fit the spectrum and correct for the dust attenuation in the optical range. The method of Li et al. (2020) will give a relative attenuation curve, which is shown in the left panel. After correcting for the dust attenuation, we fit the corrected spectrum with the spectrum fitting code BIGS. As shown in the right panel, the best-fit spectrum provided by BIGS is extended to both NUV and NIR (orange line). This dust-free spectrum is convolved with filter response functions to predict a dust-free SED, which is compared with the observed SED shown by red stars in the right panel. By assuming that the Ks band is not affected by dust attenuation, the observed SED is also normalized so that the flux at the Ks band is the same as the dust-free spectrum. The difference between the dust-free and observed SEDs is our attenuation estimation, which is indicated with dashed lines in the right panel.
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Left: absolute attenuation in the V band (A  V ) as a function of the sSFR. The black line shows the median relation of all of the pixels in our galaxies, and the gray and light gray shaded regions indicate the 1σ and 2σ scatter of individual spaxels around the median. The stars are the results from the stacked spectra within 1Re  of each galaxy, color-coded by the total stellar mass of the galaxy indicated by the color bar. The red/green triangles/lines show the results for subsamples of spaxels selected by b/a, the minor-to-major axis ratio of the SDSS r-band image of the host galaxies. Right: same as the left panel except that the red/green triangles/lines are for subsamples selected by the galactocentric distance of the spaxels.
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Slope of the attenuation curve in the optical (A  B /A  V ) as a function of the sSFR. The black line shows the median values of the results obtained from individual pixels, with gray shaded regions indicating 1σ and 2σ scatters of the data points. The stars are the results from the 1Re  stacks of each galaxy, with color codes showing the total stellar mass of the galaxy (from NSA). In the panels from left to right, colored triangles/lines show the results of subsamples of spaxels selected by A  V  (left), b/a (middle), and galactocentric distance (right).
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Two example galaxies in our sample. From left to right, the panels show the optical image, the Swift uvm2 image, the absolute attenuation in the V band (A  V ), the slope of the attenuation curve in the optical (A  B /A  V ), and the bump strength B in each galaxy. In each panel, the MaNGA footprint is shown in magenta, with a red plus sign marking the center of the integral field.
Paper: Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
Authors: Yi-Xian Chen, Adam Burrows, Ankan Sur, Roberto Tejada Arevalo
Figure caption: Comparison of the TP profiles of different Jupiter models at ﹩{\tilde{T}}_{\mathrm{eff}}=125﹩ K. Only the isolated (no irradiation or cloud) models show no temperature inversion. All other models are irradiated at 5.2 au, either without clouds or with clouds of modal particle size of 1 μm. We observe that P irr is closely related to the temperature valley at the inversion around 0.1 bar and that P irr = 0.15 best reproduces the observational data. Once the redistribution factor is set, the existence of clouds does not alter the TP profile. Other particle sizes also have TP profiles that nearly coincide with the green line. The Galileo entry probe data from Seiff et al. (1998) is plotted in black.
Paper: Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
Authors: Yi-Xian Chen, Adam Burrows, Ankan Sur, Roberto Tejada Arevalo
Figure caption: Left panel: evolution of internal brightness temperature T int and emission temperature T eff for our fiducial Jupiter model (blue) evolved in our adiabatic code, the Fortney et al. (2011) boundary condition (taken from their Figure 7), and the Burrows et al. (1997) boundary condition evolved in our adiabatic code. Right panel: the evolution of the model Jupiter radius. An extra evolutionary track for zero core mass is plotted with a dashed line to show that a solid core is needed to make the planet more compact.
Paper: Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
Authors: Yi-Xian Chen, Adam Burrows, Ankan Sur, Roberto Tejada Arevalo
Figure caption: The specific entropy in the convective zone under the atmosphere’s thin radiative layer, plotted as a function of gravity, and effective temperature ﹩{\tilde{T}}_{\mathrm{eff}}﹩ (red) or internal temperature T int (blue) for our fiducial model (f = 0.5, P irr = 0.15, and a 0 = 1 μm). At low temperatures, ﹩{\tilde{T}}_{\mathrm{eff}}﹩ starts to become significantly larger than T int due to the increasing contribution of stellar irradiation.
Paper: Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
Authors: Yi-Xian Chen, Adam Burrows, Ankan Sur, Roberto Tejada Arevalo
Figure caption: Left panel: Jupiter’s temperature evolution comparing different zenith angle factors f. Right panel: Jupiter’s temperature evolution comparing different cloud particle size parameters a 0.
Paper: Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
Authors: Yi-Xian Chen, Adam Burrows, Ankan Sur, Roberto Tejada Arevalo
Figure caption: Geometric albedo spectra for different irradiated atmospheric models without clouds (red) or with clouds of different modal particle sizes, fixing P irr = 0.15. The black spectrum is from Karkoschka (1998).
Paper: A Broadband X-Ray Study of the Dwarf Nova SS Cyg during Quiescence and Outburst
Authors: Anirban Dutta, Vikram Rana, Koji Mukai, Raimundo Lopes de Oliveira
Figure caption: Optical lightcurve of SS Cyg in the visual band (source: AAVSO). The epoch of simultaneous NuSTAR and XMM-Newton observations during quiescence and outburst is marked.
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: Left: Stokes I, Q, and U spectra of the region “Shell” (data points) and the best-fit model (solid lines). Right: residuals in terms of (data−model)/error. The six Stokes I spectra from two observations are coded using different colors. The six Stokes Q and U spectra are grouped for better visualization.
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: Background-subtracted Stokes I spectrum from DU1 (data points) of the region “Shell” and the background level (solid line).
Paper: Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry
Authors: Ping Zhou, Dmitry Prokhorov, Riccardo Ferrazzoli, Yi-Jung Yang, Patrick Slane, Jacco Vink, Stefano Silvestri, Niccolò Bucciantini, Estela Reynoso, David Moffett, Paolo Soffitta, Doug Swartz, Philip Kaaret, Luca Baldini, Enrico Costa, C.-Y. Ng, Dawoon E. Kim, Victor Doroshenko, Steven R. Ehlert, Jeremy Heyl, Frédéric Marin, Tsunefumi Mizuno, Melissa Pesce-Rollins, Carmelo Sgrò, Toru Tamagawa, Martin C. Weisskopf, Fei Xie, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovčiak, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Silvia Zane
Figure caption: Stokes I image overlaid with regions E–H with decreasing brightness.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Simulated transit spectra of cloudy super-Earths using YunMa. Solid line: total transit depth with all contributions included. Dotted–dashed line: water ice clouds. Faint-dotted line: water vapor. Blue, green, and red lines: H2/He-dominated, cloudy atmospheres with different p c (see legend). Purple and yellow lines: heavier cloudy atmospheres with 50% N2.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Retrieval posteriors for cases (22) (purple), (23) (orange), and (24) (green) in Table 2. Blue crosses indicate the ground truth parameters, and the vertical dashed lines in histograms indicate the 1σ and 2σ confidence ranges of the posterior distribution. These three retrievals use the same transit spectrum as input (thin cloud with ﹩{X}_{{{\rm{N}}}_{2}}﹩ = 0.5 in Figure 6) but different retrieval assumptions. Case (22) (purple): H2O and N2 are included as priors, and the cloud formation is simulated by YunMa. Case (23) (orange): same as case (22) except that N2 is not included among the priors. Case (24) (green): same as case (22) except that the cloud is simulated by a simpler model from TauREx, in which the atmosphere becomes opaque below the cloud deck. The only retrieved cloud parameter for the simpler model is the cloud deck pressure, which is not shown here for simplicity.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Retrieved T–p profile of case (22) in Table 2. The isothermal temperature (T c), surface temperature (T surf), and the pressure where the isothermal profile starts (p c) are retrieved using YunMa and indicated by squares in the plot. The solid purple line indicates the two-point profile fitted from the retrieved T c, T surf, and p c values. The shaded area indicates the standard deviation of the posterior distribution. We also plot a T–p profile with an isothermal upper atmosphere, a DALR-estimated lower atmosphere and a MALR-estimated cloud-forming region to show how the two-point profile can deviate from the adiabatic lapse rate (ALR) when similar cloud cover forms. The two-point profile is a useful approximation to estimate cloud formation while reducing the retrieval computing time.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Test results for r c (top left), N (top right), and the transit spectrum (bottom) with different sedimentation efficiency f sed. The cloud layer shrinks with the increasing of f sed.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Example of numerical instability in cloud formation simulations when large relative (rtol) and absolute (atol) tolerances are chosen in solving Equation (2) with Runge–Kutta method. Blue plots: rtol=1 × 10−8, and atol = 1 × 10−12. Red plots: rtol = 1 × 10−12, and atol = 1 × 10−15. In these tests, the retrieval performances are affected by numerical instability, as illustrated in this figure where multiple islands of solutions in the posteriors are clearly visible.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption: Example of cloud retrieval using YunMa integrated in TauREx 3 (case (2) in Table 2). The sedimentation efficiency (f sed), which is the main parameter controlling the cloud microphysics, is well recovered together with the vapor water mixing ratio.
Paper: YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds
Authors: Sushuang Ma, Yuichi Ito, Ahmed Faris Al-Refaie, Quentin Changeat, Billy Edwards, Giovanna Tinetti
Figure caption:  YunMa retrieval experiments with thick clouds and ﹩{X}_{{{\rm{N}}}_{2}}﹩ = 0.5 (orange line in Figure 6). Observational uncertainty = 10 ppm (blue line, case (27) in Table 2) and = 1 ppm (brown line, case (28) in Table 2). Red lines indicate GTPs.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption:  J dependence of the S μ 2 ratio between the experiment and the calculation based on the two databases, JPL and CDMS, derived for the J 3 − J 2 A−+ v t = 0 transitions of CH3OH. The measured transition frequencies are also compared with calculated values in the JPL database, which are superposed in blue. The calculated frequencies in JPL agree with the values in CDMS on the order of kHz.
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: (a) and (b) Radio spectra from RFS/LFR for 14 days around Encounter 1 and Encounter 15, respectively. (c) and (d) Obtained plasma frequency f pe overplotted on the RFS/LFR spectra for Encounter 1 and Encounter 15, respectively. (e) and (f) Obtained electron density n e for Encounter 1 and Encounter 15, respectively.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: The ratios of S μ 2 obtained in this study and those calculated based on the CDMS and the JPL database for the J  K  = 50 − 40 transitions of CH3OH. A and E indicate the symmetry of the torsional state. v t indicates the quantum number of the torsional vibration.
Paper: Laboratory Measurement of CH2DOH Line Intensities in the Millimeter-wave Region
Authors: Takahiro Oyama, Yuki Ohno, Akemi Tamanai, Yoshimasa Watanabe, Satoshi Yamamoto, Takeshi Sakai, Shaoshan Zeng, Riouhei Nakatani, Nami Sakai
Figure caption: Ratios between the derived S μ 2 values and the calculated ones for the b-type Q-branches in 13CH2DOH.
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: (a) Relation between retrieved f pe and n e with error bars intrinsic due to limited frequency resolution of RFS/LFR. (b) Relative error on density as a function of obtained plasma density, demonstrating the suitability of RFS/LFR measurements above 80 kHz or 80 cm−3.
Paper: Quasi-thermal Noise Spectroscopy Analysis of Parker Solar Probe Data: Improved Electron Density Model for Solar Wind
Authors: Oksana Kruparova, Vratislav Krupar, Adam Szabo, Marc Pulupa, Stuart D. Bale
Figure caption: A 2D histogram of obtained electron density as a function of radial distance from the Sun based on 2,115,146 data points obtained during the first 15 encounters by Parker Solar Probe. The power-law fit is shown as a solid black line.