adsabs/AstroCLIMB huggingface dataset:
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Depiction of some perturbed transitions in the v27 = 1 and v26 = 1 states. The y-axis depicts the difference between the transition frequency in the excited and ground vibrational state, scaled by J″ + 1. All transitions are b-type R-branch lines. The scatter points depict the measured transitions. The red and blue lines connect each of the scatter points in order to more clearly display the perturbation. For the values without points, either the ground state or the excited state transition occurred at a frequency that was not measured in our experiment.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Transitions of 3-hydroxypropanal with the highest signal-to-noise ratio in the GOTHAM DR5 data toward TMC-1. The simulated line profile (red) is overlaid on top of the observational data (gray). The spectrum is simulated at the 3σ upper limit column density of 8.6 × 1011 cm−2. The other simulation parameters are detailed in the text and Table 4.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: The structures and relative zero-point-corrected energies (in kJ mol−1 and kT-equivalent temperature) of the four most stable conformers of 3-hydroxypropanal. The dipole moments are listed as μa/μb/μc. The point group of each conformer is also shown. See text for computational details. The red spheres denote oxygen atoms, the gray spheres are carbon atoms, and the white spheres depict hydrogen atoms.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: The strongest simulated lines of 3-hydroxypropanal in the observational data toward NGC 6334I. The simulated line profile (red) is overlaid on top of the observational data (gray). The spectrum is simulated at the 3σ upper limit column density of 4.2 × 1016 cm−2. The other simulation parameters are detailed in the text and Table 4.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Column density ratio of acetaldehyde to 3-hydroxypropanal in each of the sources analyzed in this work. The arrows denote a column density upper limit of 3-hydroxypropanal. The values used for this figure and the related references are listed in Table 4.
Paper: Low-latitude Sunspot Group Tilt Angles in 15–24 Activity Cycles
Authors: Andrey G. Tlatov
Figure caption: Relationship between the parameters of bipoles at latitudes θ < θcut and the amplitude of the next SNn activity cycle: (a) for MWOMF data and the parameter ﹩{\overline{\sin \theta \cdot {\gamma }^{\theta }}}_{n-1}{\rm{\Sigma }}{S}_{n-1}^{\theta }﹩ for θ < θcut = 14﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2; (b) for MWOMF data and the slope parameter μ for θcut = 14﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2; (c) same as (a) for KK data and θcut = 9﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4; (d) same as (b) for KK data and θcut = 9﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4; (e) same as (a) for MWO data for θcut = 8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5; and (f) same as (b) for MWO data for θcut = 8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5. The dashed line shows the linear approximation.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots of best-fit Sonora (left) and Phoenix (right) model temperature vs. IR spectral type. The markers are color coded by spectral type. The size of the markers corresponds to the number of objects represented by each point. The temperatures plotted are the mean temperatures yielded after 100 Monte Carlo (MC) resamples. Error bars come from the standard deviation of all 100 fits and are only shown when nonzero. The six gray star markers denote objects in the sample with unknown errors and thus undetermined uncertainty to their fit temperatures. The Sonora temperatures generally decrease, but plateau through the L–T transition. The Phoenix temperatures suggest a similar trend, but the scatter in temperature through the L types as well as the limited temperature range make the plateau less clear.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Box plots showing the distribution of the differences between the best-fit values of T eff found in this work (Sonora models on top and Phoenix models on the bottom) and those found in SANGHI23 for the 247 objects shared by both samples. In their paper, SANGHI23 find the best-fit T eff using forward-model fits to the ATMO models (left) and also derive T eff values using evolutionary models (right). In each case, the SANGHI23 temperatures are subtracted from the temperatures found in this work.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Scatterplots (left) and box plots (right) showing the distribution of the best-fit cloud parameters (f sed for the Sonora models and grain size/pressure at the top of the cloud deck for the Phoenix models) vs. IR spectral type. The scatterplot markers are color coded by spectral type and sized according to the number of objects they represent. Parameter values and error bars were obtained by performing 100 MC resamples of each spectrum and finding the mean and standard deviation of the resulting fits, respectively. The increasing trends in all three parameters indicate that silicate clouds fall deeper in the atmosphere through the L–T sequence, but are still high enough to influence the near-IR spectrum through the late T types.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots of best-fit Sonora (left) and Phoenix (right) model temperature vs. J − K color, color coded by IR spectral type. Again, the temperatures and error bars come from the 100 MC resampling results, and only the nonzero errors are shown. The gray stars again denote the objects with unknown uncertainties. There is a trend of general reddening with later spectral type until the L–T transition, where colors quickly become bluer. The larger uncertainties and truncated temperature range make this trend more difficult to see for the Phoenix fits as compared to the Sonora fits.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Box plots showing the distribution of best-fit gravity vs. IR spectral type for the Sonora (left) and Phoenix (right) model fits. The mean value for each spectral type bin is given in red. The two model sets give entirely different trends in log(g), suggesting that surface gravity fit results to the near-IR are model dependent and poorly constrained.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The left scatterplot shows the best-fit metallicity [M/H] vs. best-fit temperature of the objects in our sample. The markers are color coded by IR spectral type and sized based on the number of objects they represent. The values of [M/H] and temperature are averages after 100 MC resamples for each object. Uncertainties are also calculated based on the resampling results. The right bar plot shows the best-fit [M/H] vs. IR spectral type. The mean [M/H] for each bin is depicted in red. Both plots show a decrease in [M/H] with decreasing temperature/later type.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Box plots showing the distribution of the differences between the best-fit values of log(g) found in this work (Sonora models on top and Phoenix models on the bottom) and those found in SANGHI23 for the 247 objects shared by both samples. In their paper, SANGHI23 find best-fit log(g) using forward-model fits to the ATMO models (left) and also derive log(g) values using evolutionary models (right). In each case, the SANGHI23 log(g) values are subtracted from the values found in this work.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Histograms showing the distribution of objects that were best fit by Bobcat (blue), Cholla (orange), or Diamondback (green) models. The plots show the distribution by (a) IR spectral type, (b) best-fit temperature, and (c) (J − K)2MASS color index. Nearly every object in our sample was best fit by a Diamondback model.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Histograms showing the distribution of best-fit mixing (Kzz ) vs. IR spectral type for the Sonora (a), Cholla only (b), and Phoenix (c) model fits. A suite of models with a full grid of cloud and mixing parameters is needed to better analyze vertical mixing.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: The SpeX spectrum (black) of each blue early T object is shown with its uncertainty (gray) and best-fit Sonora (blue dashed) and Phoenix (orange dashed) models. The first four digits of the R.A. coordinates of each object are given to the left. A reference spectrum made by averaging all T1–T2 objects from the sample is included at the bottom of the plot. The reference spectrum is plotted on top of each object, roughly scaled so the J-band fluxes match. Note that all members of this family are overluminous in J band relative to their K-band peaks. J1435 is the exception, but its K band has very large uncertainty. This object was included in the family because of its very blue 2MASS J − K color.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: Plots showing the best binary model fits to the five members of the blue early T family. The models are all Sonora models. The data and composite models are plotted in black and green, respectively, The orange and blue curves give the individual components that were summed together to generate the composite model. The parameters of the two component models are given in Table 8.
Paper: A Survey of Model Fits to Brown Dwarf Spectra Through the L–T Sequence
Authors: Savanah K. Turner, Denise C. Stephens, Conner B. Scoresby, Josh A. Miller
Figure caption: 2MASS J − K color is plotted against IR spectral type. The blue early T objects are marked in red at the top of the general sample (gray). The members of this family are all T1 or T2s and are blue for their spectral types.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Best solutions of the polarization decomposition using BISP-1 with optical (first two rows) and NIR (last two rows) polarization observations in the regions of C5 (left), C45 (middle), and C50 (right). The first and third rows show the Stokes parameters q(v, h) and u(v, h) as a function of the distance modulus calculated using the inverse parallax. The red vertical lines and shaded areas represent the cloud median distances and their 1σ and 2σ confidence intervals. Similarly, the horizontal solid lines and shaded areas represent the LOS-integrated median q(v, h) (green) and u(v, h) (purple) and their 1σ and 2σ uncertainties for each group of stars behind the polarizing layers. The bottom panels show the extinction per distance unit (10−3 mag pc−1) profiles from J. L. Vergely et al. (2022) at 10 pc (gray) and 50 pc (light-gray) resolution; the distance of the profiles is on a logarithmic scale. The second and fourth rows show the posterior distributions of the inverse parallax for each cloud modeled. The vertical dashed lines show the median values.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Polarization maps of star groups located behind each BISP-1 layer in C5 (top), C45 (middle), and C50 (bottom). The insets in the top right show the distribution of the polarization angle observed along with the median value (the red line) and the average magnetic field orientation from Planck (the blue line, also shown as a pseudovector in the center of the map). The median polarization properties of the components obtained with BISP-1 are shown in the top left of the panels (also see Table 1). The red ruler shows the actual spatial scale measured for an angular scale of ﹩0\mathop{.}\limits^{^\circ }1﹩ at the distance of the clouds.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Starlight polarization observations from IPS-GI (in white) and GPIPS (in black) catalogs, after filtering, in the regions C5, C45, and C50. The colored background is the column density obtained using the thermal dust optical depth maps at 353 GHz from Planck Collaboration Int. XLVIII et al. (2016). The white texture in the background represents the plane-of-sky GMF orientation as observed by Planck (Planck Collaboration XII et al. 2020), and it is generated using line integral convolution (LIC, B. Cabral & L. Leedom 1993).
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Optical (the orange dots) and NIR (the blue dots) debiased polarization degree as a function of the distance for stars common to both surveys in regions C5, C45, and C50 (from top to bottom, respectively). The dashed orange and blue lines show the median polarization degree, and the solid lines show the weighted mean per distance bin. The shaded areas represent the 68% confidence intervals. The polarization (right axis) is compared with optical extinction per parsec (AV pc–1, left axis) from J. L. Vergely et al. (2022), at 10 pc (the solid gray curve) and 50 pc (the solid light-gray curve) resolution. The extinction density units are 10−3 mag pc−1. Bottom row: polarization maps for stars common to IPS-GI (orange) and GPIPS (blue) in the same regions. The gray squares mark the approximate limits of the IPS-GI field of view.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top row: ratio of the degree of polarization in the optical to NIR as a function of distance of stars in common between the IPS-GI and GPIPS observations in each region. Bottom row: systematic difference between the NIR and optical polarization angles as a function of the distance in each region. The horizontal blue dashed line is the mean value of the distribution shown in the right-side panels. The solid dark-orange lines represent the mean and standard deviation per distance bin. The weighted circular mean and standard deviation were used in the case of the angular difference.
Paper: Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, V. Pelgrims, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Illustration of the observed starlight polarization produced by two clouds with different magnetic field properties.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: The ratio of integrated flux density to peak flux density of the sources detected in the CHILES Con Pol survey (left panel) and histograms and fractions of unresolved and resolved sources (right panel) as a function of flux density. (A) The resolved sources based on the integrated to peak flux ratio are shown with blue filled triangles, while the unresolved sources are shown with red filled squares. The horizontal black dashed line indicates the unity ratio. The typical (median) uncertainty in this ratio (σ = 0.18) and 10% flux density are shown in the upper left of the plot. (B) Histograms of unresolved sources (blank red bars) and resolved sources (filled light blue bars) are shown with a bin size of ﹩{\rm{\Delta }}\mathrm{log}\,{S}_{1.4\mathrm{GHz}}=0.2﹩. The percentage of unresolved sources (red dashed line) and resolved sources (blue solid line) are also shown.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: The ratio of flux densities of between the MIGHTEE and CHILES Con Pol catalogs as a function of the CHILES Con Pol 1.4 GHz flux density. Panels (A) and (B) show comparisons of the CHILES Con Pol sources with the R = 0 MIGHTEE catalog, while panels (C) and (D) present the comparisons with the R = −1.2 MIGHTEE catalog. Panels (A) and (C) illustrate the ratio of flux densities with their uncertainties, and panels (B) and (D) show the same data as hexbin plots. In panels (A) and (C), red symbols indicate the weighted mean in each bin with uncertainties, and horizontal lines show the range of bins. The orange dashed curves for the R = 0 catalog (top rows) show that our estimated catalog completeness is 20 μJy (∼12σ) while it is 30 μJy (5σ) for the R = −1.2 catalog (bottom rows).
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: Euclidean-normalized radio source counts including those of the CHILES Con Pol 7σ catalog sources (black squares). Published source counts by other recent surveys are also shown for comparison: C. L. Hale et al. (2023) for the COSMOS field (green triangles), A. M. Matthews et al. (2021) for the DEEP2 field (red downside triangles) and NVSS (blue hexagram), T. Mauch et al. (2020) for the DEEP2 field (blue circles), and G. de Zotti et al. (2010) for a compilation of surveys with gray circles. The models estimated from our P(D) analysis are also displayed for comparison: the CHILES Con Pol (Paper I) as the blue solid line, the DEEP2 field (T. Mauch et al. 2020) as the red dashed line, and NVSS (A. M. Matthews et al. 2021) as the orange dotted line.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: Hexbin plots (2D histograms) of the radio spectral index as a function of 1.4 GHz power (panel (A)) and zbest (panel (B)). The red line indicates the linear regression computed by a robust linear model (lmRob function) in R (R Core Team 2013).
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: Derived 1.4 GHz power of individual sources is shown as a function of redshift in the left panel while the same distribution is shown as a hexbin plot in the right panel to reflect the source density better. In the left panel, green open squares and black open diamonds represent spec-z sources with and without an estimated spectral index, respectively. Black-filled triangles and red upside-down triangles represent phot-z sources with and without an estimated spectral index. The three lines delineate 7σ detection limits for the three different assumed spectral indices: α = −1 (solid), 0 (dotted), and +1 (dashed).
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: The ratio of flux densities of the VLA-COSMOS sources with respect to those of the CHILES Con Pol sources as a function of CHILES Con Pol 1.4 GHz flux density. The left panel shows a comparison of CHILES Con Pol with VLA-COSMOS (E. Schinnerer et al. 2010) and the right panel shows the same data in a hexbin plot to include the source density information better. Red diamonds in the left panel indicate the weighted mean in each bin, same as in Figure 8. The orange dashed curves represent the boundaries of the flux density ratios, determined by the sensitivity limit (60 μJy at 5σ) for the VLA-COSMOS survey.