adsabs/AstroCLIMB huggingface dataset:
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: The mass and radius inferred using two different models for CO (ExoMol using the “.broad” file and HITEMP2019). The astrometric mass is shown in the blue shaded region (Lazorenko & Sahlmann 2018). The dashed lines show the isogravity lines.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Prior (left) and posterior (right) sampling of the layer-by-layer temperature model (green lines). The solid black lines indicate the best-fit power-law model in Section 5.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Mock spectrum of a self-luminous planet as observed by HDC (plus symbols) and the mean and 90% credible area by exojax (blue shaded area). The bottom panel shows the residuals of the median of the predictions from the data.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Difference between hjert (this paper) and scipy.special.wofz, following Grimm et al. (2021).
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Comparison of ﹩{ \mathcal T }(x)﹩ and ﹩1-{ \mathcal T }(x)﹩ using AS70 (Abramowitz & Stegun 1970; Heng et al. 2014; Lavie et al. 2017) + JAX (ours, exojax.rtransfer.trans2E3) with scipy.special.expn. The bottom panel shows the difference (﹩| { \mathcal T }(x)(\mathrm{ours})-{ \mathcal T }(x)(\mathrm{scipy})| ﹩). The dot and cross symbols correspond to F32 and F64. The horizontal dashed line indicates 2 × 10−7.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Comparison of exojax.special.erfcx (ours) with scipy.erfcx for x > 0.0.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Comparison of MODIT F32 and F64 with the direct LPF.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Definitions of physical quantities in the atmospheric layers.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Pressure points with the largest contribution to the radiation at the line centers of CO (left) and H2O (right). We assumed an isothermal atmosphere with T = 1700  K and log g = 5. The green line corresponds to the largest contribution of the CIA (H2–H2).
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Map of the sky with the blazars in the BZCAT5, BROS, and CRATES catalogs plotted with black, gray, and green dots, respectively. BZCAT5 objects with R-band catalog magnitudes brighter than 15.5, which is the median maximum saturation magnitude in the LSST r band, are highlighted with blue circles. The regions enclosed by red lines represent the planned DDFs—from north to south, these are: COSMOS, XMM-LSS, ECDFS, ELAIS S1, and EDFS (the double field).
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: (a) Median values over the sky of the maximum (blue squares), median (black dots), and minimum (red diamonds) saturation magnitudes over the 10 yr period of the survey for the different Rubin-LSST filters. The filled symbols refer to the OpSim run baseline_nexp2_v1.7_10yrs, which include two exposures of 15 s each per visit; the unfilled symbols refer to baseline_nexp1_v1.7_10yrs, with a single exposure of 30 s per visit. Histogram (b) and sky map (c) of the maximum saturation magnitude in the r band for the nexp2 cadence simulation.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Left: parameter distributions for the flaring sources used in the saturation metric. From top left, clockwise: the R-band catalog magnitudes adopted for “off-flare” brightness levels; the outburst amplitudes (mag); the plateau times (days); and the periods (days). Right: the top panel shows the percentage of detected sources (red) and the percentage of sources detected in outburst (blue), while the bottom panel shows the percentage of saturated observations for the various OpSim runs listed on the right.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Left: sky map of 2029 simulated blazars. Values of 1 denote they would be detected brightening by 0.5 mag in the baseline strategy, values of zero mean there would be no detection. Right: the fraction of observations per source that would be saturated.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: The number of observations (left) and the number of color indices obtained by coupling the data from two bands taken in the same night (right) at the end of the 10 yr survey. Values have been obtained using the baseline_nexp2_v1.7_10yrs OpSim run. The black triangles refer to the DDFs, while the other symbols and colors refer to the WFD, in three different positions in the sky.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: The minimum time separations (in days) between the observations in two different filters for the WFD (left) and the DDFs (right). Values have been obtained using the baseline_nexp2_v1.7_10yrs OpSim run. Different colors are used for different filter pairs, and the horizontal width of each pair is proportional to the corresponding number of points, in order to better distinguish the number density. The black crosses indicate mean values.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Left: the BVRI light curves of the blazar 3C 454.3 processed by the WEBT. The red line in the R-band panel represents a cubic spline interpolation through the 4 day binned light curve. The red lines in the other panels represent the same cubic spline interpolation, shifted according to average color indices. Right: the simulated Rubin-LSST sampling, according to TransitAsciiMetric, with a 10 yr baseline cadence. The blue diamonds refer to the WFD, while the green plus signs refer to the DDFs. The gray symbols indicate the WEBT data shown in the left panel.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Time separations (minutes) between the subsequent observations of the DDFs in the same filter. The different colors distinguish different bands, as indicated in the legend. The left panel refers to the baseline_nexp2_v1.7_10yrs cadence simulation, and the right panel refers to the daily_ddf_v1.5_10yrs one.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Color indices as a function of brightness (left) and time (right). The gray circles and blue diamonds represent real WEBT and simulated WFD colors, respectively. All of them have been obtained by coupling data with time separations of less than 1 hr. The red dashed line indicates the mean color index derived from the WEBT data. The accumulation of blue points close to the average level is explained in the text. The black lines are linear and parabolic fits to the WEBT data, highlighting the redder-when-brighter trend, with the “saturation” effect at the bright end. All plots have the same amplitude Δ index = 1.2 mag to make the comparison between the colors easier. A few outliers, deviating more than 3σ from the mean, have been discarded.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Color indices as a function of brightness (left) and time (right). The gray circles and green plus signs represent the real WEBT and simulated DDF colors, respectively. All of them have been obtained by coupling data with time separations below 1 hr. The red dashed line indicates the mean color index derived from the WEBT data. The accumulation of green points close to the average level is explained in the text. The black lines are linear and parabolic fits to the WEBT data, highlighting the redder-when-brighter trend, with the “saturation” effect at the bright end. All plots have the same amplitude Δ index = 1.2 mag to make the comparison between the colors easier. A few outliers, deviating more than 3σ from the mean, have been discarded.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Difference between the numbers of WFD visits in various cadence simulations and that of the baseline_nexp2_v1.7_10yrs cadence. OpSim runs with either double 15 s (left) or single 30 s (right) exposure times per visit are shown.
Paper: Blazar Variability with the Vera C. Rubin Legacy Survey of Space and Time
Authors: Claudia M. Raiteri, Maria I. Carnerero, Barbara Balmaverde, Eric C. Bellm, William Clarkson, Filippo D'Ammando, Maurizio Paolillo, Gordon T. Richards, Massimo Villata, Peter Yoachim, and Ilsang Yoon
Figure caption: Difference between the numbers of DDF visits in various cadence simulations and that of the baseline_nexp2_v1.7_10yrs cadence. OpSim runs with either double 15 s (left) or single 30 s (right) exposure times are shown.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The sky distribution of the galaxies in the Final Release of the 6dF Galaxy Survey.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Redshift distributions of the full 6dF sample, 2MRS–6dF subsample (dark gray), and the faint 6dF subsample. To distinguish the different samples of the different sets of 6dF galaxies, we call the whole 6dF as full 6dF, the subset of 6dF data in 2MRS is 2MRS–6dF, and the 6dF galaxies that are not in the 2MRS and are fainter are faint 6dF. Redshifts are adopted from Jones et al. (2004, 2009).
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Distribution of the mean S/N of the full 6dF spectra (light gray), 2MRS–6dF spectra (dark gray), and faint 6dF spectra (white). To distinguish the different samples of the different sets of 6dF galaxies, we call the whole 6dF the full 6dF, the subset of 6dF data in 2MRS is 2MRS–6dF, and the 6dF galaxies that are not in the 2MRS and are fainter are faint 6dF.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: S/N of the subsamples vs. wavelength. To distinguish the different samples of the different sets of 6dF galaxies, we call the whole 6dF that full 6dF, the subset of 6dF data in 2MRS is 2MRS–6dF, and the 6dF galaxies that are not in the 2MRS and are fainter are faint 6dF. We define the S/N in each wavelength bin as the data divided by the error provided in the error spectrum. The symbols are the mean and the error bars are the standard deviation of the S/N distributions.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Sample spectra of the 6dF data. Left column shows spectra of emission-line galaxies, right column shows spectra of non-emission-line galaxies. Mean S/N increases from top to bottom.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The Type 2 AGNs in our catalog requiring that the [O I] line has S/N ≥ 2.0 in addition to the four main AGN identification lines, i.e., Hα, Hβ, [O III] λ5007, and [N II] λ6584. The orange dots are AGNs and the black dots are non-AGNs according to the [N II]/Hα criteria from Kewley et al. (2001). The red line shows the [O I] AGN demarcation line and the blue dashed line shows the Sy2 vs. LINERs line from Kewley et al. (2006).
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The Type 2 AGNs in our catalog requiring the [SII] line to have an S/N ≥ 2.0 in addition to the four main AGN identification lines, i.e., Hα, Hβ, [O III] λ5007, and [N II] λ6584. The orange dots are AGNs and the black dots are non-AGNs according to the [N II]/Hα criteria from Kewley et al. (2001). The red line shows the [SII] AGN demarcation line and the blue dashed line shows the Sy2 vs. LINERs line from Kewley et al. (2006).
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The sky distribution of the AGN catalog from 6dF Type 1 (broadline) AGNs and Type 2 (narrowline) AGNs satisfying the Kauffmann et al. (2003) criteria. The Type 1 AGNs are marked as black dots.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The BPT diagrams for the emission-line galaxies ((S/N)line ≥ 2.0 for all four lines). 6dF galaxies in 2MRS are shown as orange dots for comparison. The green and red lines denote the Kauffmann et al. (2003) and Kewley et al. (2001) criteria for narrow line AGNs, respectively.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Mean S/N of the AGN sample as a function of redshift. The mean value in each redshift bin is shown as a square. Error bars are the standard deviations of each bin.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: The Type 2 AGNs in our catalog, separated into Seyferts (purple) and LINERs (green) using the Kewley et al. (2006) criteria. There are more LINERs than Seyferts in the 2MRS–6dF subsample (Ks ≤ 11.75), and more Seyferts than LINERS in the faint 6dF subsample (Ks ≤ 12.65) due to the lower data quality. LINERs have weaker emission lines, so they are preferentially lost when spectral S/N decreases, i.e., the faint 6dF galaxies. Note that we use the [O III]/Hβ vs. [N II]/Hα BPT diagram to identify AGNs, so some emission-line galaxies that do not qualify as AGNs in the main diagram appear in the AGN region in the [O III]/Hβ vs. [S II]/Hα diagram.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: AGN fraction (left column) and distribution (right column) as a function of the continuum S/N. The S/N of R-band spectra is assessed for Type 1 AGNs and the S/N of V-band spectra is assessed for Type 2 AGNs. The top row is for Type 1 AGNs, the middle row is for Type 2 AGNs satisfying the Kewley et al. (2001) criteria, and the bottom row is for Type 2 AGNs satisfying the Kauffmann et al. (2003) criteria. The AGN fraction increases with S/N and saturates at S/N ≳ 40; beyond this value, the AGN fractions for the different subsamples are consistent with each other.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Left panel: ratio of the number of identified AGNs to the number of galaxies in our spectroscopic sample (Nsample), across the southern sky. The sky has been divided into 768 equal-area regions, and the color indicates the AGN fraction. Right panel: 6dF AGN fraction as a function of redshift. In these plots, we have combined the broadline AGNs with the narrowline AGNs that satisfy the Kauffmann et al. (2003) criteria. The Nsample includes the spectra free from telluric contamination and a few hundred spectra with strong broad Hα emission components that are affected by the telluric absorption.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Left panel: ratio of the number of identified AGNs weighted by likelihood to the number of galaxies in 6dF, across the southern sky. The sky has been divided into 768 equal-area regions, and the color indicates the AGN fraction. Right panel: statistically weighted AGN fraction distribution as a function of redshift. The homogeneous AGN fraction across the southern sky and in redshift is shown in the statistically weighted 6dF AGN catalog. We have combined the broadline AGNs with the narrowline AGNs that satisfy the Kewley et al. (2001) criteria in these plots.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Left panel: ratio of the number of identified Type 1 (Sy1) AGNs to the number of Type 2 (K01) AGNs in 6dF, across the southern sky. The sky has been divided into 768 equal-area regions, and the color indicates the AGN fraction. Right panel: Type 1 (Sy1) to Type 2 (K01) AGN fraction distribution as a function of redshift.
Paper: A Uniformly Selected, Southern-sky 6dF, Optical AGN Catalog
Authors: Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal
Figure caption: Left panel: ratio of the number of Type 1 (Sy1) AGNs to the number of Type 2 (K01) AGN likelihood in 6dF assigned based on continuum S/N across the southern sky. The sky has been divided into 768 equal-area regions, and the color indicates the AGN fraction. Right panel: the statistically weighted Type 1 (Sy1) to Type 2 (K01) AGN fraction distribution as a function of redshift. The nearly homogeneous Type 1 (Sy1) to Type 2 (K01) AGN fractions across the southern sky and in redshift are seen in the statistically weighted 6dF AGN catalog.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: (a) The block diagram of the system. (b) The prototype of the system.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: (a) The feed radiation patterns at 35 (black), 37 (red), and 40 (purple) GHz. (b) The prototype of feed with the secondary reflector. (c) The antenna radiation pattern at 35.25 GHz, the main lobe is ∼0.8°. (d) The prototype of the antenna-feed system.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: The design diagram of the AFE.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: (a) The designed diagram of the digital receiver. The daughterboard transmitted the time-domain data to the FPGA on the motherboard by JESD204B. The motherboard completed the digital signal processing: deframing, the Hanning window, 8k-point fast Fourier transform (FFT), square root, and integration are finished in the FPGA, while packaging, timestamping, and uploading are accomplished in the digital signal processor (DSP). (b), (c) The prototype of the receiving system.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: The input of ADC hardware design. The single-ended input is converted to a differential input by Balun to suppress common-mode interference.
Paper: A Broadband Solar Radio Dynamic Spectrometer Working in the Millimeter-wave Band
Authors: Shang ZiQian, Xu Ke, Liu Yang, Wu Zhao, Lu Guang, Zhang YuanYuan, Zhang Lei, Su YanRui, Chen Yao, and Yan FaBao
Figure caption: The diagram of the 8k-point FFT algorithm for each channel of the ADCs (Channel A for example). Data in the time domain is divided into eight subgroups. Data in each group is then processed with a Hanning window and 1k-point FFT. The final three-step butterfly operation uses FPGA logic resources to accelerate the operation.