adsabs/AstroCLIMB huggingface dataset:
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: Power spectra for a 32-channel simulated image with all noise sources active except the ROIC amplifier terms, before and after c = 4 phantom-pixel correction. The 1/f component here is from Video8 and bias noise. While subdominant to the ROIC noise, these sources of 1/f noise are mitigated by phantom-pixel corrections.
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: Side-by-side comparison of a measured (left) and simulated (right) N = 74 32-channel image pair difference. Each image has S = 24 row chopping and r = 32 distributed reference correction.
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) Example output 32-channel N = 74 noise realization generated by the described simulation and (b) corresponding spatial power spectrum, with phantom-pixel correction but without reference pixel correction. Large channel offsets due to low-frequency 1/f noise are visible prior to reference correction.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for four PPNs: the Red Rectangle illuminated by HD 44179 (Geballe et al. 1985), CRL 2688 (Geballe et al. 1992), IRAS 04296+3429 (Geballe et al. 1992), and IRAS 05341+0852 (Geballe & van der Veen 1990).
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Aliphatic and aromatic C–H stretching features of four PDRs (IRAS 18416-0420, Jourdain de Muizon et al. 1990; Orion Bar, Sloan et al. 1997; IRAS 19442+2427, Jourdain de Muizon et al. 1990; S106, Geballe et al. 1985). The observed spectra are shown as black diamonds. The fitted spectra (solid red lines) are a combination of two or more Drude profiles and a linear, underlying continuum.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for six sources of which the effective temperatures of the illuminating stars are unknown: IRAS 16362-4845 (Jourdain de Muizon et al. 1990), IRAS 06572-0742 (Jourdain de Muizon et al. 1990), IRAS 09296+1159 (Geballe & van der Veen 1990), IRAS 12063-6259 (Jourdain de Muizon et al. 1990), IRAS 17199-3446 (Jourdain de Muizon et al. 1990), and IRAS 19097+0847 (Jourdain de Muizon et al. 1990).
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for four external galaxies: M82 (Yamagishi et al. 2012), NGC 253 (Yamagishi et al. 2012), NGC 2782 (Onaka et al. 2018), and LMC (Mori et al. 2012).
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 5 but for aliphatic PAH cations.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for four planetary nebulae (IC 418, Geballe et al. 1985; BD+303639, Geballe et al. 1985; IRAS 21282+5050, Jourdain de Muizon et al. 1986; NGC 7027, Geballe et al. 1985).
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for the reflection nebulae NGC 1333 (Joblin et al. 1996) and IRAS 03035+5819 (Jourdain de Muizon et al. 1986).
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Histogram of the aliphatic fractions of PAHs for 28 UIE sources. The median aliphatic fraction is 〈η ali〉 ≈ 5.4%.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 7 but for four YSOs (IRAS 20293+3952, IRAS 20319+3958, IRAS 19213+1723, and IRAS 03260+3111; Jourdain de Muizon et al. 1990).
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 magnetic field for the aligned flow case. Top row: the frequency spectra of the magnetic island, forward Alfvén, fast, and slow magnetosonic modes (left); and the spectra of the magnetic island and backward Alfvén, fast, and slow magnetosonic modes (right). The dashed black line in each plot is a reference f −5/3 curve. Middle row: the parallel wavenumber spectra of the forward and backward Alfvén mode magnetic field fluctuations (left), the parallel wavenumber spectra of parallel wavenumber spectra of the parallel and perpendicular components, and the total magnetic field fluctuations of the fast magnetosonic modes (middle); the parallel wavenumber spectra of the parallel and perpendicular components, as well as the total magnetic field fluctuations of the slow magnetosonic modes (right). Bottom row: the perpendicular wavenumber spectra of the magnetic island and forward and backward Alfvén mode magnetic field fluctuations (left), the perpendicular wavenumber spectra of the parallel and perpendicular components, and the total magnetic field fluctuations of the fast magnetosonic modes (middle); and the perpendicular wavenumber spectra of the parallel and perpendicular components, as well as the total magnetic field fluctuations of the slow magnetosonic modes (right).
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 magnetic field for the highly oblique case. Top row: the frequency spectra of the magnetic island, forward Alfvén, fast, and slow magnetosonic modes (left); and the frequency spectra of the magnetic island and 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 magnetic field fluctuations of the fast magnetosonic modes (middle); and the parallel wavenumber spectra of the parallel and perpendicular components, as well as the total magnetic field fluctuations of the slow magnetosonic modes (right). Bottom row: the perpendicular wavenumber spectra of the magnetic island and forward and backward Alfvén mode magnetic field fluctuations (left); the perpendicular wavenumber spectra of the parallel and perpendicular components, as well as the total magnetic field fluctuations of the fast magnetosonic modes (middle); and the perpendicular wavenumber spectra of the parallel and perpendicular components, as well as the total magnetic field fluctuations of the slow magnetosonic modes (right).
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. 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 velocity 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 velocity 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).
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 for the aligned case showing separately the contributions to the normalized fluctuating magnetic field from top to bottom. Left column: the forward and backward fast ﹩\delta {B}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the forward and backward x-components of the Alfvén mode ﹩\delta {B}_{x}^{A\pm }﹩ and the magnetic island mode ﹩\delta {B}_{x}^{i}﹩. 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 magnetic island mode ﹩\delta {B}_{y}^{i}﹩. 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 for the highly oblique case, showing separately the contributions to the normalized fluctuating magnetic field from top to bottom. Left column: the forward and backward fast ﹩\delta {B}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the x-component of the magnetic island and forward and backward Alfvén mode ﹩\delta {B}_{x}^{i,A\pm }﹩. Right column: the forward and backward slow ﹩\delta {B}_{z,y,x}^{s\pm }﹩ magnetosonic modes, respectively, and the y-component of the magnetic island and forward and backward Alfvén modes ﹩\delta {B}_{y}^{i,A\pm }﹩. 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 over the highly oblique 30 minute interval showing the density fluctuations. Top row, left to right: the frequency spectra of the entropy, forward fast and slow, and backward fast and slow magnetosonic modes, δ ρ  e , δ ρ  f±, and δ ρ  s±. Bottom left: from top to bottom, the entropy mode and the forward and backward fast and slow magnetosonic modes. Bottom right: PSDs in isotropic wavenumber k of the entropy and forward-propagating (top) and backward-propagating magnetosonic modes (bottom). 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: Overview of a 30 minute highly oblique slow solar wind interval observed by the Solar Orbiter spacecraft on 2020 August 12. From top to bottom, we plot the magnitude of the magnetic field ∣B∣, the components of the magnetic field (left axis and black curves) and velocity field (right axis and blue curves) in the RTN coordinate system, the angle θ  BV  between the magnetic and flow velocity vectors, the proton number density, and the proton plasma beta β  p .
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 for the aligned case, showing separately the contributions to the normalized fluctuating velocity from top to bottom. Left column: the forward and backward fast ﹩\delta {u}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the forward and backward x-components of the Alfvén mode ﹩\delta {u}_{x}^{A\pm }﹩. Right column: the forward and backward slow ﹩\delta {u}_{z,y,x}^{s\pm }﹩ magnetosonic modes, respectively, and the forward and backward y-components of the Alfvén mode ﹩\delta {u}_{y}^{A\pm }﹩. All fluctuating quantities are normalized to the mean flow 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 in the mean-field coordinates for the highly oblique case, showing separately the contributions to the normalized fluctuating velocity from top to bottom. Left column: the forward and backward fast ﹩\delta {u}_{z,y,x}^{f\pm }﹩ magnetosonic modes, respectively, and the forward and backward x-components of the Alfvén mode ﹩\delta {u}_{x}^{A\pm }﹩. Right column: the forward and backward slow ﹩\delta {u}_{z,y,x}^{s\pm }﹩ magnetosonic modes, respectively, and the forward and backward y-components of the Alfvén mode ﹩\delta {u}_{y}^{A\pm }﹩. All fluctuating quantities are normalized to the mean flow speed as labeled.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the y band.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the NB1010 images.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the CHORUS NBs (left: NB527, middle: NB718, right: NB973).
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the r band.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the z band.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the NB921 images.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the g band.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the NB816 images.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the i band.
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 luminosity (L X) vs. temperature (kT) of the X-ray-emitting plasma in groups (black squares) and clusters (black circles) of galaxies (Mulchaey 2000). Group data are from Xue & Wu (2000) and Helsdon & Ponman (2000), while data of clusters are from Wu et al. (1999). The X-ray luminosities have been rescaled to the cosmology adopted in the present analysis. In this figure we represent with red and blue circles the properties of the X-ray-emitting gas surrounding B2.1 0742+31 and B2.3 2254+35, respectively. Full colored circles indicate the results from the spectra extracted from the whole diffuse X-ray emission, while empty colored circles indicate the results from the spectra extracted from the regions that exclude the extended radio structures.
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: Hard-band 3–7 keV Chandra ACIS-S flux maps for sources in the present sample that show evidence of extended X-ray emission (see Section 3.1). The VLASS 3 GHz contours overlaid in green are the same ones from Figure 1.
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: Pan-STARRS (Chambers et al. 2016) r  P1 filter image of B2.1 0742+31, with overlaid in blue the 150 MHz TGSS contours from Figure 1. Black crosses indicate, in addition to the galaxy hosting the radio source, field sources with redshift measurements close to that of B2.1 0742+31 (0.461). The redshift value is indicated next to each cross.
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: The calibrated solar radio flux at 37.25 GHz in various weather conditions (fog on March 8, sunny to cloudy on March 12, cloudy to rain on May 28, cloudy on May 29, cloudy on May 30, cloudy to sunny on June 2, and sunny on July 7). The system was calibrated five times by observing the solar background, and the cold and hot noise sources, using the first calibration parameters before 2:00:00, the second calibration parameters between 2:00:00 and 4:00:00, and so on. However, there is a gap (as shown by the pink circles) at each calibration caused by freshly selecting the sky background, changes in solar pitch angle, and the slow change in the system transmission slope. Until 02:00:00, the data were calibrated using the first set of calibration parameters, resulting in no gap at 0:00:00. Based on a measured solar brightness temperature of 11,636 K, a flux of approximately ∼3000–4000 SFU was derived. This differs significantly from the NoRP measurement. NoRP sets the flux at 2400 SFU for the quiet Sun, relying only on observations of the solar background at regular intervals without any additional calibration.
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) Slope tests for system transmission based on the noise source were performed every 6 minutes during regular observations. Values below 2500 (the system output power, without calibration) are the output of the Sun, the solar background, and the cold of the noise source feeding into the system. (b) After opening the temperature control for an hour, the calibration unit was stabilized at 20°C. The gain changes quickly before the temperature of the calibration unit stabilizes (at 22:00:00). The figure suggests that the room-temperature component of the AFE is affected by the external ambient temperature, causing the slope of the system to fluctuate slowly depending on the AFE’s room temperature, and it can be seen that the slope is lowest at around 06:00, due to the high external temperature at midday, while the slope rises in the morning and evening when the temperature is low. This variation in slope introduces a consistency bias that might be improved on summer days and days with low temperature differences, while daily observations reduce the effect of slope variation through periodic calibrations.
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) Solar brightness temperature at 37.25 GHz is obtained using the new-Moon calibration in 2023 February and March. (b) The correction factor C(ν) was measured multiple times in February and March, with a CV of 5.3%. The deviation of the correction factor C(ν) can lead to an overall high or overall low for F sun(ν) in the range 35–40 GHz.
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) Block diagram of the AFE with a noise source and temperature controller, utilizing the waveguide form to decrease noise. (b) A real item of the upgraded calibration unit with the thermoelectric cooler for thermostatic control, which is currently maintained at a constant temperature of 20°C due to limited cooling power.