adsabs/AstroCLIMB huggingface dataset:
Paper: The Chaotic History of the Retrograde Multi-planet System in K2-290A Driven by Distant Stars
Authors: Sergio Best, and Cristobal Petrovich
Figure caption: Nodal precession frequencies ﹩{\dot{{\rm{\Omega }}}}_{{\rm{s}},\mathrm{bc}}﹩ (red lines), ﹩{\dot{{\rm{\Omega }}}}_{\mathrm{bc},{\rm{s}}}﹩ (blue lines) and ﹩{\dot{{\rm{\Omega }}}}_{\mathrm{bc},{\rm{B}}}﹩ (green lines and shaded region) for the example in Figure 2(b) comparing two cases: mutual inclination iB,C = 10° (no ZKL cycles; dashed lines) and iB,C = 85° (ZKL cycles, solid lines). Panel (a): dependence on the initial mutual inclination iB,C with the shaded green region displaying the whole possible range for ﹩{\dot{{\rm{\Omega }}}}_{\mathrm{bc},{\rm{B}}}\propto {\left[1-{e}_{{\rm{B}}}^{2}\right]}^{3/2};﹩ resonances are only encountered for iB,C ≳ 50°. Panel b: time evolution showing the resonance crossings that occur only for initial iB,C = 85° (solid lines). Panel c: evolution of the stellar obliquity showing that the sudden changes coincide with resonance crossings. The case with initial iB,C = 10° without resonance crossing have only small periodic changes.
Paper: The Chaotic History of the Retrograde Multi-planet System in K2-290A Driven by Distant Stars
Authors: Sergio Best, and Cristobal Petrovich
Figure caption: Fraction of the time that the system spends with an inclination of 124 ± 6 within the system’s age (3.2–5.6 Gyr). Parameters where set according to Figure 1, while varying the stellar inclinations (vertical axes) and J2 in a broad range. The red vertical lines indicate the current values of J2 for Love numbers k2 of 0.01 and 0.02. Panel (a): case without star C. Panels (b) and (c): case with star C with fractions as a function of the initial values of ibc,B and iB,C, respectively. The white lines correspond to the limiting condition to cross the resonances in Equation (10) and the horizontal ones correspond to the limit in which the system is destroyed because star B approaches too close to the inner planets (aB[1 − eB] ≈ ac).
Paper: The Chaotic History of the Retrograde Multi-planet System in K2-290A Driven by Distant Stars
Authors: Sergio Best, and Cristobal Petrovich
Figure caption: Fraction of the systems that reach the observed angle of 124° in our population synthesis study described in Section 3.2. Overall, the success rate is 56%, while in 17% of the systems the planets are destroyed and 27% never reach ≥124° (if we only consider the systems that are not destroyed, the success rate goes up to 67%). From panels (a) to (f) we show the fractional dependence on: initial period of the star, final value of J2, mutual inclination of B and C, mass of planet b, and semimajor axis of stars B and C. The red marks in panel (b) correspond to a case without star C for comparison where the success rate is only 12% and the initial distribution of eB (not shown) is largely skewed to very large values with a mean of 0.86.
Paper: Strong H2O and CO Emission Features in the Spectrum of KELT-20b Driven by Stellar UV Irradiation
Authors: Guangwei Fu, David K. Sing, Joshua D. Lothringer, Drake Deming, Jegug Ih, Eliza Kempton, Matej Malik, Thaddeus D. Komacek, Megan Mansfield, and Jacob L. Bean
Figure caption: The emission spectrum of KELT-20b (black) is overplotted with the ATMO retrieval best-fit model (purple), PHOENIX forward model (pink), and blackbody model of 2402K (gray). The blue shaded regions represent 1–3σ uncertainties from ATMO retrieval. The TP profiles are shown on the right with corresponding colors for ATMO and PHOENIX best-fit models. The blue shaded region represents 1σ uncertainties. Contribution functions from ATMO for each wavelength channel are overplotted with dashed lines. The data probe pressure levels range from 100 to 1 mbar with TESS being the lowest and the blue side of WFC3/G141 (1.1–1.3 μm) being the highest. We detected prominent H2O and CO emission features indicating a strongly inverted TP profile as shown by both models. The excellent agreement of the TP profiles between ATMO and PHOENIX shows the day-side atmosphere is or very close to radiative equilibrium.
Paper: Strong H2O and CO Emission Features in the Spectrum of KELT-20b Driven by Stellar UV Irradiation
Authors: Guangwei Fu, David K. Sing, Joshua D. Lothringer, Drake Deming, Jegug Ih, Eliza Kempton, Matej Malik, Thaddeus D. Komacek, Megan Mansfield, and Jacob L. Bean
Figure caption: KELT-20b emission spectrum metrics compared with other hot Jupiters with day-side temperatures higher than 2200 K overplotted with PHOENIX models assuming solar metallicity and C/O ratio. The top panel shows the water feature strength metric ﹩{{\rm{S}}}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ from Mansfield et al. (2021) and KELT-20b is located in a unique parameter space of high host-star temperature combined with low day-side temperature. The large water emission feature from KELT-20b is consistent with the PHOENIX model predictions. The bottom panel shows the Spitzer 4.5 μm blackbody brightness temperature relative to the WFC3/G141 out-of-water band blackbody brightness temperature. The large difference between the two bands in KELT-20b indicates a prominent CO emission feature.
Paper: Strong H2O and CO Emission Features in the Spectrum of KELT-20b Driven by Stellar UV Irradiation
Authors: Guangwei Fu, David K. Sing, Joshua D. Lothringer, Drake Deming, Jegug Ih, Eliza Kempton, Matej Malik, Thaddeus D. Komacek, Megan Mansfield, and Jacob L. Bean
Figure caption: Posterior distribution of ATMO retrieval. The retrieved metallicity, carbon, and oxygen abundances are ∼3.9, 10, and 17 times higher than the solar values, but the retrieved C/O ratio of ﹩{0.454}_{-0.205}^{+0.211}﹩ is consistent with the solar value to within one sigma. The log(g) is not well constrained as the emission spectrum is not sensitive to surface gravity.
Paper: Helium Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
Authors: N. Marcelli, M. Boezio, A. Lenni, W. Menn, R. Munini, O.P. M. Aslam, D. Bisschoff, M.D. Ngobeni, M.S. Potgieter, O. Adriani, G.C. Barbarino, G.A. Bazilevskaya, R. Bellotti, E.A. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A.M. Galper, S.V. Koldashov, S. Koldobskiy, A.N. Kvashnin, A.A. Leonov, V.V. Malakhov, L. Marcelli, M. Martucci, A.G. Mayorov, M. Mergè, E. Mocchiutti, A. Monaco, N. Mori, V.V. Mikhailov, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S.B. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y.I. Stozhkov, A. Vacchi, E. Vannuccini, G.I. Vasilyev, S.A. Voronov, Y.T. Yurkin, G. Zampa, and N. Zampa
Figure caption: Left panel: the evolution of the helium energy spectrum as intensities approached the period of maximum solar activity, from 2010 January (violet) to 2014 September (red). Right panel: the ratio of the measured spectra with respect to the spectrum of 2010 January. The color code is the same as the right panel.
Paper: Helium Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
Authors: N. Marcelli, M. Boezio, A. Lenni, W. Menn, R. Munini, O.P. M. Aslam, D. Bisschoff, M.D. Ngobeni, M.S. Potgieter, O. Adriani, G.C. Barbarino, G.A. Bazilevskaya, R. Bellotti, E.A. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A.M. Galper, S.V. Koldashov, S. Koldobskiy, A.N. Kvashnin, A.A. Leonov, V.V. Malakhov, L. Marcelli, M. Martucci, A.G. Mayorov, M. Mergè, E. Mocchiutti, A. Monaco, N. Mori, V.V. Mikhailov, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S.B. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y.I. Stozhkov, A. Vacchi, E. Vannuccini, G.I. Vasilyev, S.A. Voronov, Y.T. Yurkin, G. Zampa, and N. Zampa
Figure caption: Top: PAMELA helium spectra measured in 2011 and late 2013 compared with the corresponding AMS-02 measurements (Aguilar et al. 2018), as indicated in the legend. The AMS-02 fluxes were averaged over three Carrington rotations. Bottom: the ratios between PAMELA and AMS-02 fluxes. A constant fit was performed on the ratios and the results (P0) are shown in the legend.
Paper: Helium Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
Authors: N. Marcelli, M. Boezio, A. Lenni, W. Menn, R. Munini, O.P. M. Aslam, D. Bisschoff, M.D. Ngobeni, M.S. Potgieter, O. Adriani, G.C. Barbarino, G.A. Bazilevskaya, R. Bellotti, E.A. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A.M. Galper, S.V. Koldashov, S. Koldobskiy, A.N. Kvashnin, A.A. Leonov, V.V. Malakhov, L. Marcelli, M. Martucci, A.G. Mayorov, M. Mergè, E. Mocchiutti, A. Monaco, N. Mori, V.V. Mikhailov, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S.B. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y.I. Stozhkov, A. Vacchi, E. Vannuccini, G.I. Vasilyev, S.A. Voronov, Y.T. Yurkin, G. Zampa, and N. Zampa
Figure caption: Time profiles of proton-to-helium ratio for the five rigidity intervals specified in the legend. The error bars are the quadratic sum of statistical and systematic errors. After 2009 the data points cover nine Carrington rotation time periods. The lines and P0 parameters resulting from the fit of a constant in each rigidity bin in the solar minimum (solid line) and maximum (dashed line) periods are also shown.
Paper: Helium Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
Authors: N. Marcelli, M. Boezio, A. Lenni, W. Menn, R. Munini, O.P. M. Aslam, D. Bisschoff, M.D. Ngobeni, M.S. Potgieter, O. Adriani, G.C. Barbarino, G.A. Bazilevskaya, R. Bellotti, E.A. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A.M. Galper, S.V. Koldashov, S. Koldobskiy, A.N. Kvashnin, A.A. Leonov, V.V. Malakhov, L. Marcelli, M. Martucci, A.G. Mayorov, M. Mergè, E. Mocchiutti, A. Monaco, N. Mori, V.V. Mikhailov, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S.B. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y.I. Stozhkov, A. Vacchi, E. Vannuccini, G.I. Vasilyev, S.A. Voronov, Y.T. Yurkin, G. Zampa, and N. Zampa
Figure caption: Time profile of the proton-to-helium ratio at the rigidity intervals listed in the legend, normalized to the mean value of the ratios in the solar maximum period from 2013 May to 2014 September. The error bars are the quadratic sum of statistical and systematic errors. A weighted average over 9 months (with the exception of the last point before 2010, which is a weighted average over 10 months) was performed to reduce statistical fluctuation and the effect of the short-term cyclic variation in the solar minimum period. The AMS-02 data (Aguilar et al. 2018), normalized over the same solar maximum period, are shown for the period after 2014 September. The dashed lines are the proton-to-helium ratios and their corresponding uncertainties, colored bands, derived using the force-field approximation for solar modulation as described in Section 4.
Paper: Helium Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
Authors: N. Marcelli, M. Boezio, A. Lenni, W. Menn, R. Munini, O.P. M. Aslam, D. Bisschoff, M.D. Ngobeni, M.S. Potgieter, O. Adriani, G.C. Barbarino, G.A. Bazilevskaya, R. Bellotti, E.A. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A.M. Galper, S.V. Koldashov, S. Koldobskiy, A.N. Kvashnin, A.A. Leonov, V.V. Malakhov, L. Marcelli, M. Martucci, A.G. Mayorov, M. Mergè, E. Mocchiutti, A. Monaco, N. Mori, V.V. Mikhailov, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S.B. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y.I. Stozhkov, A. Vacchi, E. Vannuccini, G.I. Vasilyev, S.A. Voronov, Y.T. Yurkin, G. Zampa, and N. Zampa
Figure caption: Proton (top set of lines) and helium-nuclei (lower lines) fluxes (J) measured by the PAMELA experiment from 2006 June (violet) to 2014 September (red) divided by rigidity squared vs. kinetic energy divided by the charge (Ze). The displacements along the abscissa are similar between the two species and they are attributed to the varying with time of the solar modulation parameter.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Profile of the difference of Gaussian kernel (black curve) that is convolved with the original image to produce a filtered image with the large-scale background removed and the visibility of the filaments enhanced. The kernel is the difference of a narrow Gaussian (σ1 = 2.5 pixels; red curve) and a wider Gaussian (σ2 = 4.5 pixels; blue curve).
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Top (2a): a mosaic image of the Galactic center at 20 cm with a 4″ resolution taken with MeerKAT (Heywood et al. 2022). Prominent sources are labeled. The names of the filaments are taken from (LaRosa et al. 2001; Yusef-Zadeh et al. 2004; Law et al. 2008). The rms noise in this image ∼80 mJy beam−1. This data product is publicly available in Heywood et al. (2022). Bottom (2b): a filtered version of (a) with rms sensitivity of 1.8–2.3 μJy and a resolution of 6.″4. The units of the filtered image do not account for the changed beam size. The subtraction built into the filtering reduces the apparent intensities by a factor of ∼0.13.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Top (a): an image of the spectral index for pixels with sufficient signal in the filtered image(s) to yield a reliable estimate. Bottom (b): an image showing the spectral index (see color bar) for filaments longer than 132″. For reference, the spectral index values are superimposed on a grayscale image of the intensity.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Left (a): histogram of the number of filaments as a function of spectral index for linear features longer than 66″. Two Gaussian components were fit to the data suggesting steep spectrum nonthermal linear features (red) and flat thermal H II regions (light blue). Right (b): similar to (a) except long filaments > 132″ were selected.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: (a): A scatter plot of the spectral index as a function of absolute values of latitude for linear features longer than 66″. The red line is a χ2 fit to the data with a slope shown to the top right. (b): Similar to (a) except only for filaments longer than 132″ were selected, to exclude virtually all H II structures and most SNR shock structures.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: The equipartition magnetic field as a function of spectral index using different ranges of electron energies. The dotted blue lines shows the result when it is assumed that α = −0.5 (i.e., Equation (1) instead of Equation (2)). Plotted results corresponds to brightness Iν = 1 mJy arcsec−2 and thickness L = 1″.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Top (a): an image of the distribution of the equipartition magnetic field assuming all the features are nonthermal emission and have a spectral index α = −0.5, as calculated from Equation (1). Bottom (b): equipartition magnetic field calculated from Equation (2), employing the measured spectral indices. In this image, features with α > −0.4 have been masked.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Left (a): histogram of the number of filaments as a function of the magnetic field for linear features longer than 66″. The variation of spectral index has been accounted for. Right (b): similar to (a) except long filaments >132″.
Paper: Statistical Properties of the Population of the Galactic Center Filaments: the Spectral Index and Equipartition Magnetic Field
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood, W. Cotton, and F. Camilo
Figure caption: Left (a): histogram of the number of filaments as a function of median surface brightness for linear features longer than 66″. The red line indicates a power-law fit to the bright portion of the histogram, indicating a power-law index of k = −0.75. Right (b): similar to (a) except long filaments >132″ were selected to exclude virtually all H II structures and most SNR shock structures.
Paper: Submillimeter Pulsations from the Magnetar XTE J1810-197
Authors: Pablo Torne, Graham S. Bell, Dan Bintley, Gregory Desvignes, David Berry, Jessica T. Dempsey, Paul T. P. Ho, Harriet Parsons, Ralph P. Eatough, Ramesh Karuppusamy, Michael Kramer, Carsten Kramer, Kuo Liu, Gabriel Paubert, Miguel Sanchez-Portal, and Karl F. Schuster
Figure caption: XTE J1810−197 detection with JCMT/SCUBA-2 at ν ≈ 353 GHz (λ = 0.85 mm). The upper three panels show the results from 2020 February 27, the three middle panels from 2020 July 9, and the three bottom panels from 2021 May 15. In each case, the total integration time was folded with a resolution of 50 maps over the spin period of the magnetar (P ≈ 5.54 s), thus with a time resolution of 110.8 ms. For each epoch, the panels show: (left) average of the three maps containing the pulsation from the neutron star, (center) average of 39 maps during the off-pulse time (those separated at least 4 maps from the 3 maps containing the ON signal), and (right) resulting image after subtracting the off-pulse average map from the on-pulse average, showing the residual of the on-pulse emission from XTE J1810−197. The telescope beam size is shown in the lower left corner on each panel. For 2021 May 15, the On–Off map is smoothed with a matched filter with primary Gaussian component of 11″ to improve the visualization of the residual.
Paper: Submillimeter Pulsations from the Magnetar XTE J1810-197
Authors: Pablo Torne, Graham S. Bell, Dan Bintley, Gregory Desvignes, David Berry, Jessica T. Dempsey, Paul T. P. Ho, Harriet Parsons, Ralph P. Eatough, Ramesh Karuppusamy, Michael Kramer, Carsten Kramer, Kuo Liu, Gabriel Paubert, Miguel Sanchez-Portal, and Karl F. Schuster
Figure caption: Average pulse profiles of the magnetar XTE J1810−197 at the different frequency bands. The top three panels show the detections at 353 GHz (λ = 0.85 mm). Each profile includes the telescope, frequency, date of observation, and averaged flux density in the legends. The time resolution is adapted to improve the signal-to-noise ratio, being 43.3 ms (128 bins) between 209 and 353 GHz, 21.6 ms (256 bins) between 86 and 154 GHz, and 2.7 ms (2048 bins) at 6 GHz. The profiles were manually aligned to the peak of the main component.
Paper: Submillimeter Pulsations from the Magnetar XTE J1810-197
Authors: Pablo Torne, Graham S. Bell, Dan Bintley, Gregory Desvignes, David Berry, Jessica T. Dempsey, Paul T. P. Ho, Harriet Parsons, Ralph P. Eatough, Ramesh Karuppusamy, Michael Kramer, Carsten Kramer, Kuo Liu, Gabriel Paubert, Miguel Sanchez-Portal, and Karl F. Schuster
Figure caption: Mean profile of the magnetar XTE J1810−197 at 353 GHz (λ = 0.85 mm) after averaging the profiles from the observations of 2020 February 27, 2020 July 9, and 2021 May 15 from the JCMT.
Paper: Submillimeter Pulsations from the Magnetar XTE J1810-197
Authors: Pablo Torne, Graham S. Bell, Dan Bintley, Gregory Desvignes, David Berry, Jessica T. Dempsey, Paul T. P. Ho, Harriet Parsons, Ralph P. Eatough, Ramesh Karuppusamy, Michael Kramer, Carsten Kramer, Kuo Liu, Gabriel Paubert, Miguel Sanchez-Portal, and Karl F. Schuster
Figure caption: Spectral fits for XTE J1810−197. The upper panel shows single power-law fits, and the bottom panel a broken power law. In both panels, the triangle markers show the centimeter-averaged flux densities from Effelsberg at 4.5, 5.5, 6.5, and 7.5 GHz on 2020 July 8, the circles show the millimeter-averaged flux densities from the IRAM 30 m telescope at 86, 102, 138, 154, 209, and 225 GHz on 2020 July 10, and the black square the averaged flux density from the detection from JCMT at 353 GHz on 2020 July 9. The purple star and orange diamond represent the averaged flux density measured at 353 GHz on 2020 February 27 and 2021 May 15 for comparison, but they are not used for the power-law fits. 1σ error bars are shown, but are often smaller than the size of the symbols. The black, purple, and orange down-pointing arrows at 666 GHz mark the 3σ upper flux density limits for our observations from the JCMT on 2020 July 9, 2020 February 27, and 2021 May 15, respectively. The top panel shows three different single power-law fits: the blue dotted line using only the IRAM 30 m data, the dotted–dashed green line is the fit to a combination of millimeter and submillimeter data, and the dashed red line shows the single power-law fit to all data from 2020 July combined. See Sections 3 and 4 and Table 2 for details.
Paper: Submillimeter Pulsations from the Magnetar XTE J1810-197
Authors: Pablo Torne, Graham S. Bell, Dan Bintley, Gregory Desvignes, David Berry, Jessica T. Dempsey, Paul T. P. Ho, Harriet Parsons, Ralph P. Eatough, Ramesh Karuppusamy, Michael Kramer, Carsten Kramer, Kuo Liu, Gabriel Paubert, Miguel Sanchez-Portal, and Karl F. Schuster
Figure caption: Comparison of the standard (left panel) and custom (right panel) SCUBA-2 daisy maps. The red and blue squares represent the position on the focal plane of the good bolometers in the 850 and 450 μm bands, respectively. The black line shows the position of the center of the target during a ∼2 min scan in each of the two scan patterns. The standard daisy pattern utilizes all the eight subarrays (four at each wavelength band 850 and 450 μm) to cover a large field of view. The custom smaller daisy pattern was adapted to minimize interruptions of the time streams, i.e., to avoid as much as possible bad bolometers and obtain the maximum number of data points for a point-like source like the magnetar. The calibration of the data was verified to be consistent between the two observing modes within 1.7%.
Paper: Eccentric Dust-ring Formation in Kozai–Lidov Gas Disks
Authors: Rebecca G. Martin, and Stephen H. Lubow
Figure caption: Eccentricity, argument of periapsis, inclination, and nodal phase-angle evolution of the gas (blue lines) and dust (red lines) in time at a semimajor axis of a = 20 au.
Paper: Eccentric Dust-ring Formation in Kozai–Lidov Gas Disks
Authors: Rebecca G. Martin, and Stephen H. Lubow
Figure caption: Evolution of the dust and gas disk in time during one KL oscillation. The green circle shows the primary star. The secondary star is along the x axis but is not shown on this scale. The red points show SPH gas particles while the blue points show the dust particles. Each row shows the disk from two viewing angles, the x–z plane (left) and the y–z plane (right). The rows show times t = 0, 7.6, 9.5, 12.3 and 21.4 Porb from top to bottom.