adsabs/AstroCLIMB huggingface dataset:
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: The X-ray image (left panel), smoothed with a Gaussian kernel of 42.″426, for the radio source G4Jy 1863. Radio contours are drawn using a radio map at 843 MHz starting at the level of 90 mJy beam−1 and increasing by a factor of 3. Black circles, of 20 pixel radius, mark the location of point-like sources detected at an S/N < 3, while blue arrows mark the locations of both the northern (N) and the southern (S) radio lobe. The X-ray counterpart of the radio core (S1) and that of the nearby companion galaxy (S2) have a clear counterpart in the optical (r-band) image retrieved from DES r band (central panel) as well as at mid-IR frequencies at 3.4 μm obtained with the Wide-field Infrared Survey Explorer (WISE) All-sky survey (right panel). X-ray intensity contours, obtained from the Swift-XRT event files and drawn starting at a level of 0.01 photons, are overlaid onto both the optical and the mid-IR images to help identifying the location of the low-energy counterparts to S1 and S2. The X-ray emission of both the northern and the southern radio lobes is detected, above a 3σ level of confidence, comparing the number of photons measured within a circular region, of 20 pixel radius, centered on their radio intensity peak and that expected, on average, on a background region of the same area.
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: Left panel: the X-ray image of G4Jy 1192 obtained from the merged XRT event file smoothed with a Gaussian kernel of 10 pixels (i.e., 23.″57), as in Figure 2 and in Figure 7, with radio contours drawn from the TGSS radio map overlaid. These contours were computed starting at level of 0.1 Jy beam−1 and increase in level by a binning factor of 4. Middle and right panels: the same field but observed as part of the WISE All-sky survey at 3.4 μm and in the red filter collected from the DSS archive, respectively. The magenta dashed circle in the left panel is centered on the location of the X-ray counterpart to mark its position, the same is marked by the blue dashed circles in the other two panels, while the cyan cross marks the location of the radio source (i.e., brightness-weighted radio centroid) as reported in the G4Jy catalog. In our previous analysis (Paper I) G4Jy 1192 lacks both mid-IR and optical counterparts. However, thanks to the Swift-XRT analysis, we have been able to identify these counterparts. X-ray contours obtained from the image in the left panel are overlaid onto both the mid-IR and optical images for comparison.
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: Upper panels: the left image is obtained from the merged XRT event files, smoothed with a Gaussian kernel of 10 pixels (i.e., 23.″57), as in Figure 2, while the right one is the optical image retrieved from the DSS archive in the red filter. The blue circle in the right panel is centered on the location of the X-ray counterpart to mark its position and that of the corresponding host galaxy. Radio contours are overlaid onto both images drawn at the frequency indicated (i.e., 843 MHz obtained from the SUMSS archive) together with the intensity of the first contour level and increasing in level by a binning factor of 2. Lower panels: same as the upper panels but for the radio source G4Jy 1432. Thanks to this optical-to-X-ray comparison we have been able to distinguish which source is the optical counterpart for these two radio sources having radio maps with insufficient angular resolution to locate precisely the radio core. The cyan cross marks the location of the radio source (i.e., brightness-weighted radio centroid as reported in the G4Jy catalog) while the red cross marks the mid-IR-assigned counterpart, associated in the analysis of the G4Jy sample.
Paper: The Multiwavelength Environment of Second Bologna Catalog Sources
Authors: A. Paggi, F. Massaro, H. Penã-Herazo, V. Missaglia, A. Jimenez-Gallardo, F. Ricci, S. Ettori, G. Giovannini, F. Govoni, R. D. Baldi, B. Mingo, M. Murgia, E. Liuzzo, F. Galati
Figure caption: X-ray 0.3–7 keV nuclear fluxes vs. 3 GHz radio nuclear specific fluxes for the sources for which both estimates are available (see Section 3.1). Upper limits on X-ray fluxes are represented with triangles pointing down. The red line indicates the linear regression to the logarithmic data that include the highly piled-up source B2.1 0742+31 (indicated with a red circle), while the light red shaded area represents the 1σ uncertainty around the best-fit relation. The blue line and light blue shaded area represent the linear regression and uncertainty for the logarithmic data that exclude B2.1 0742+31.
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: Left panels: Swift-XRT images. Right panels: Chandra images obtained from event files restricted in the 0.5–7 keV energy range. Radio contours at different frequencies are overlaid in black onto the Swift images and in cyan in both panels. The frequency of the radio maps from which the radio contours were drawn are reported in each panel together with the intensity of the first level and the binning factor.
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: Same as Figure 3 but for G4Jy 1664. The radio morphology of G4Jy 1664 is typical of FR II radio sources at 3 GHz, while it appears a bit extended at lower frequencies where the double radio structure does not appear.
Paper: Noise Reduction Methods for Large-scale Intensity-mapping Measurements with Infrared Detector Arrays
Authors: Grigory Heaton, Walter Cook, James Bock, Jill Burnham, Sam Condon, Viktor Hristov, Howard Hui, Branislav Kecman, Phillip Korngut, Hiromasa Miyasaka, Chi Nguyen, Stephen Padin, Marco Viero
Figure caption: (a) Overview of the SPHEREx readout electronics and (b) internal schematic of a single Video8 preamplifier channel, one of eight on the chip. Differential input lines are capacitively coupled to a low-noise integrator, and the output is read with one of two sample and hold circuits. The Video8 input can be switched to a reference voltage intermittently to track amplifier drift.
Paper: Noise Reduction Methods for Large-scale Intensity-mapping Measurements with Infrared Detector Arrays
Authors: Grigory Heaton, Walter Cook, James Bock, Jill Burnham, Sam Condon, Viktor Hristov, Howard Hui, Branislav Kecman, Phillip Korngut, Hiromasa Miyasaka, Chi Nguyen, Stephen Padin, Marco Viero
Figure caption: Illustration of row chopping on an example grid for S = 4, with black arrows representing the first pass through the array and red arrows representing the second. A predefined number of rows (here, four) are skipped over after reading each row, with a return to the first unread row every time the bottom of the array is reached.
Paper: Noise Reduction Methods for Large-scale Intensity-mapping Measurements with Infrared Detector Arrays
Authors: Grigory Heaton, Walter Cook, James Bock, Jill Burnham, Sam Condon, Viktor Hristov, Howard Hui, Branislav Kecman, Phillip Korngut, Hiromasa Miyasaka, Chi Nguyen, Stephen Padin, Marco Viero
Figure caption: Illustration of the H2RG readout operated in 32-channel mode, truncated to four channels. Each channel is read simultaneously, row by row, progressing downward. The array has a surrounding border of reference pixels 4 pixels wide. We vary the sequence of row order for improved noise stability.
Paper: Noise Reduction Methods for Large-scale Intensity-mapping Measurements with Infrared Detector Arrays
Authors: Grigory Heaton, Walter Cook, James Bock, Jill Burnham, Sam Condon, Viktor Hristov, Howard Hui, Branislav Kecman, Phillip Korngut, Hiromasa Miyasaka, Chi Nguyen, Stephen Padin, Marco Viero
Figure caption: Simulated spatial power spectra realizations corresponding to each noise component power spectrum applied to a 2048 × 2048 image obtained in readout order, with no dark current. The ROIC amplifier noise dominates at all spatial frequencies. The prominent peak at high k for the Video8 and ROIC spectra is caused by alternating column noise and is not relevant for large-scale measurements.
Paper: Noise Reduction Methods for Large-scale Intensity-mapping Measurements with Infrared Detector Arrays
Authors: Grigory Heaton, Walter Cook, James Bock, Jill Burnham, Sam Condon, Viktor Hristov, Howard Hui, Branislav Kecman, Phillip Korngut, Hiromasa Miyasaka, Chi Nguyen, Stephen Padin, Marco Viero
Figure caption: Average noise power on ﹩\theta =5^{\prime} \mbox{--}20^{\prime} ﹩ scales (0.03 < k < 0.13 pix−1) with varying skip parameter S for five measured 32-channel N = 74 image pair differences with r = 32 reference correction. The measured optimal S of a few dozen rows is consistent with that provided by the simulated noise realizations though with significantly more variation and a higher overall noise level. A substantial decrease in large-scale noise power is observed even at small values of S.
Paper: The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Authors: ZiQian Shang, 自乾 尚, Zhao Wu, 昭 武, Yan Liu, 岩 刘, Yu Bai, 宇 白, Guang Lu, 光 路, YuanYuan Zhang, 园园 张, Lei Zhang, 磊 张, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: (a) The principle of the sensitivity test. T  h  and T  c  take nominal values of the noise source. (b) According to Equation (11), the system sensitivity ﹩{\rm{\Delta }}{T}_{\min }﹩ was obtained using noise sources for multiple tests in 2023 February and March.
Paper: The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Authors: ZiQian Shang, 自乾 尚, Zhao Wu, 昭 武, Yan Liu, 岩 刘, Yu Bai, 宇 白, Guang Lu, 光 路, YuanYuan Zhang, 园园 张, Lei Zhang, 磊 张, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Comparison of CBS and NoRP data over a long period of time (almost five months). Both select data at midday (CBS data at 4:00 UT, NoRP data at 3:00 UT).
Paper: The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Authors: ZiQian Shang, 自乾 尚, Zhao Wu, 昭 武, Yan Liu, 岩 刘, Yu Bai, 宇 白, Guang Lu, 光 路, YuanYuan Zhang, 园园 张, Lei Zhang, 磊 张, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Solar flares of magnitude M5.6, M5.8, and X1.2, with the calibrated flux minus the quiet flux before the outburst.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: PAH aliphatic fraction (η ali) vs. stellar effective temperature (T eff). PPN: protoplanetary nebula; PN: planetary nebula; RN: reflection nebula; MC: molecular cloud; PDR: photodissociated region; YSO: young stellar object.
Paper: Spectral Features of the Solar Transition Region and Chromospheric Lines at Flare Ribbons Observed with IRIS
Authors: L. F. Wang, Y. Li, Q. Li, X. Cheng, M. D. Ding
Figure caption: Observation overview of the X1.3 flare on 2022 March 30. (a) GOES 1–8 Å flux and SJI 2796 Å flux (integrated over the flare region as shown in panel (d)). (b) STIX fluxes at different energy bands. The yellow shaded area marks the time period when the attenuator works. The vertical magenta dotted lines in panels (a) and (b) indicate the start, peak, and end times of the flare. (c)–(e) HMI LOS magnetogram, SJI 2796 Å, and AIA 94 Å images around the flare peak time. The red contours mark the flare ribbons as seen in the SJI 2796 Å image with a level of 15% of the maximum intensity. The vertical yellow dashed line indicates the IRIS slit position. The two blue bars in panel (d) mark the region used to integrate the Fe XXI spectra in Figure 2(a), and the cyan cross indicates the selected position where the line profiles are shown in Figures 2(c) and (d). (f)–(i) The spectra of Mg II h, C II, Si IV, and Fe XXI along the slit at 17:37:06 UT (i.e., the flare peak time). The olive dashed lines mark the reference wavelengths of these spectral lines.
Paper: Spectral Features of the Solar Transition Region and Chromospheric Lines at Flare Ribbons Observed with IRIS
Authors: L. F. Wang, Y. Li, Q. Li, X. Cheng, M. D. Ding
Figure caption: (a) Temporal evolution of the Fe XXI spectra integrated over the region outlined by two blue bars in Figure 1(d). The vertical blue dashed line indicates the reference wavelength of the Fe XXI line, and so do the vertical dashed lines in panels (b) and (c). The dark-green crosses (also in panels (b) and (c)) mark the cooler lines in the Fe XXI spectral window. The horizontal dashed lines mark the flare peak time (green) and the time (cyan) of the selected spectra in panels (b)–(d). (b) Fe XXI spectra along the slit at 17:36:10 UT. The cyan cross indicates the selected position of Y = 298.″44. (c) The observed line profile (black) at the position indicated by the cyan cross in panel (b) and its multi-Gaussian fitting (red) including the components of the Fe XXI (blue) and some cooler lines plus an unidentified line (olive). The peak intensity, Doppler velocity, and line width of the Fe XXI component and the background intensity are shown in the panel. (d) The observed Si IV line profile at the same position as the Fe XXI line profile in panel (c). Its total intensity, Doppler velocity, and line width obtained by the moment method are shown in the panel. The vertical pink dashed line indicates the reference wavelength of the Si IV line.
Paper: Spectral Features of the Solar Transition Region and Chromospheric Lines at Flare Ribbons Observed with IRIS
Authors: L. F. Wang, Y. Li, Q. Li, X. Cheng, M. D. Ding
Figure caption: Spatiotemporal variations of the total intensity (in units of log(DN)), Doppler velocity (kilometers per second), and line width (kilometers per second) of the Si IV and Mg II h lines along the IRIS slit obtained from the moment analysis. The contours indicate the flare regions with levels of (2%, 18%) and (18%, 35%) of the peak total intensities for the Si IV and Mg II h lines, respectively, with the black contour marking the main ribbon. Note that for the Si IV line we set an intensity threshold of 40 DN for a reliable S/N.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: Saturation pattern of UVOT images and definitions for the core and the wing regions. In both panels, the solid red circle with a radius of 5″ (the core of the PSF) is the standard/optimal photometric aperture of UVOT for point sources and also the point-source coincidence loss (COI) region. The dotted annulus with an inner radius of 15″ and an outer radius of 25″ is defined as the wing of the PSF. The dashed red square with a side length of 20″ represents the region heavily influenced by the COI (white square pattern) for moderate saturation. For panel (a), the raw total count rate of the wing ﹩{\dot{N}}_{\mathrm{raw},\mathrm{wing}}^{\mathrm{tot}}﹩ is ∼60 count s−1, corresponding to the case of moderate saturation, and the COI-dominated region is in the dashed square. While panel (b) shows a strongly saturated case, where ﹩{\dot{N}}_{\mathrm{raw},\mathrm{wing}}^{\mathrm{tot}}﹩ is ∼150 count s−1, and the COI-dominated region expands beyond the dashed square region. The extended source at the upper-right corner of panel (b) is an artifact (smoke ring; Page et al. 2014) caused by nearby real bright point sources. The color scale for both panels is the same.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: Normalized transmission curves of Johnson–Kron–Cousions filters and UVOT filters. Dashed lines are normalized transmission curve of the Johnson–Kron–Cousins filters, and solid lines represent those of the UVOT filters. Blue, green, and red lines represent U, B, and V bands, respectively. The effect of quantum efficiency of CCD is applied to all curves.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The additional adjustment of coincidence loss for extended sources. The horizontal axis represents the scaled raw count rate with the area ratio of the point-source COI region (25 π [arcsec2]) to the measuring region for uniform extended sources. The vertical axis represents the EXT factor (the quotient of the true incident count rate divided by the COI corrected count rate). Data is taken from Figure 6 of Breeveld et al. (2010). The point marked with a square is excluded for the fitting procedure due to its abnormal deviation from the expected value. Both the COI and EXT factors are expected to be 1 when the effect of the coincidence loss is negligible (i.e., ﹩{\dot{N}}_{\mathrm{raw},\mathrm{ext}}^{\mathrm{COI}}﹩ is ∼0 count s−1), but compared with other points, the excluded point deviates unreasonably from the expected value, which might be caused by the undisclosed large uncertainty. The vertical dotted line represents a valid threshold for the fitted model, i.e., ﹩{\dot{N}}_{\mathrm{raw},\mathrm{ext}}^{\mathrm{COI}}\lt 25\,﹩ count s−1.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The stacked image of isolated stars in the V band and one kind of segmentation of COI regions for the wing. The solid red annulus is the wing defined before. Dashed red lines are boundaries of each sector annulus with an opening angle of 22.°5. The boundaries can rotate around the center of the entire annulus with the assumption that counts distribute isotropically in the wing; hence, how to set them is arbitrary.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: The assumed coordinate system with the mean magnetic field  B  0 aligned along the z-axis and the mean flow vector  U  0 rotated into the (x, z)-plane without loss of generality, making an angle ψ with the mean magnetic field aligned z-axis.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: Overview of a fast solar wind 30 minute interval observed by the Wind spacecraft on 2020 September 28. From top to bottom, we plot the magnitude of the magnetic field ∣B∣, the x, y, z components of the magnetic field (left axis and black curves) and velocity field (right axis and blue curves) in the GSE coordinate system, the angle θ  BV  between the magnetic and flow velocity vectors, the proton number density, the plasma beta β  p , and the total pressure P  T  that is the sum of the thermal and magnetic pressure. The red vertical dashed lines identify a possible large-amplitude nonlinear structure with an enhanced ∣ B ∣ and low density.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: Mode decomposition in the mean-field coordinates showing separately the contributions to the fluctuating magnetic field from, arranged top to bottom in the left column, the forward and backward fast ﹩\delta {B}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the forward and backward x-component of the Alfvén mode ﹩\delta {B}_{x}^{A\pm }﹩ and the advected magnetic island ﹩\delta {B}_{x}^{i}﹩ (blue curve), and in the right column, the forward and backward slow ﹩\delta {B}_{z,y,x}^{s\pm }﹩ magnetosonic modes, respectively, and the forward and backward y-component of the Alfvén mode ﹩\delta {B}_{y}^{A\pm }﹩ and the advected magnetic island ﹩\delta {B}_{y}^{i}﹩ (blue). All fluctuating quantities are normalized to the mean magnetic field strength as labeled.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: Mode decomposition in the mean-field coordinates showing separately the contributions to the fluctuating velocity from, arranged top to bottom in the left column, the forward and backward fast ﹩\delta {u}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the forward and backward x-component of the Alfvén mode ﹩\delta {u}_{x}^{A\pm }﹩, and in the right column, the forward and backward slow ﹩\delta {u}_{z,y,x}^{s\pm }﹩ magnetosonic modes, respectively, and the forward and backward y-component of the Alfvén mode ﹩\delta {u}_{y}^{A\pm }﹩. All fluctuating quantities are normalized to the mean speed as labeled.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: Mode decomposition over the 30 minute interval showing separately the contributions to the fluctuating density from (top to bottom) the entropy mode and the forward and backward fast and slow magnetosonic modes, δ ρ  e , δ ρ  f±, and δ ρ  s±, respectively. All fluctuating quantities are normalized to the mean density as labeled.
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: PSD plots of the fluctuating velocity field highly oblique case. Top row: the frequency spectra of the forward Alfvén, fast, and slow magnetosonic modes (left); and the spectra of the backward Alfvén, fast, and slow magnetosonic modes (right). The dashed line in each plot is a reference f −5/3 spectrum. Middle row: the parallel wavenumber spectra of the forward and backward Alfvén mode magnetic field fluctuations (left); the parallel wavenumber spectra of the parallel and perpendicular components, as well as the total velocity field fluctuations of the fast magnetosonic modes (middle); and the parallel wavenumber spectra of the parallel and perpendicular components, as well as the total velocity field fluctuations of the slow magnetosonic modes (right). Bottom row: the perpendicular wavenumber spectra of the forward and backward Alfvén mode magnetic field fluctuations (left); the perpendicular wavenumber spectra of the parallel and perpendicular components, as well as the total velocity field fluctuations of the fast magnetosonic modes (middle); and the perpendicular wavenumber spectra of the parallel and perpendicular components, as well as the total velocity field fluctuations of the slow magnetosonic modes (right).