adsabs/AstroCLIMB huggingface dataset:
Paper: Emission-line Stacking of 21 cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
Authors: Zhaoting Chen, 兆庭 陈, Steven Cunnington, Alkistis Pourtsidou, Laura Wolz, Marta Spinelli, José Luis Bernal, Matilde Barberi-Squarotti, Stefano Camera, Isabella P. Carucci, José Fonseca, Keith Grainge, Melis O. Irfan, Mario G. Santos, Jingying Wang, 婧颖 王
Figure caption: The blue solid line shows the Fourier transformed profile of the unsymmetrized stacked spectrum (“Stacked spectrum”). The orange dashed line shows the Fourier profile of the beam ripple (“Beam ripple”). The profiles are normalized so that the maximum amplitude is 1.
Paper: Emission-line Stacking of 21 cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
Authors: Zhaoting Chen, 兆庭 陈, Steven Cunnington, Alkistis Pourtsidou, Laura Wolz, Marta Spinelli, José Luis Bernal, Matilde Barberi-Squarotti, Stefano Camera, Isabella P. Carucci, José Fonseca, Keith Grainge, Melis O. Irfan, Mario G. Santos, Jingying Wang, 婧颖 王
Figure caption: The comparison between the stacked spectra with and without the reconvolution. The blue solid line shows the stacked spectrum without the reconvolution (“No reconvolution”). The orange dashed line shows the spectrum with the reconvolution (“Reconvolution”). The vertical dashed lines show the ∣v∣ < 6500 km s−1 boundary.
Paper: Emission-line Stacking of 21 cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
Authors: Zhaoting Chen, 兆庭 陈, Steven Cunnington, Alkistis Pourtsidou, Laura Wolz, Marta Spinelli, José Luis Bernal, Matilde Barberi-Squarotti, Stefano Camera, Isabella P. Carucci, José Fonseca, Keith Grainge, Melis O. Irfan, Mario G. Santos, Jingying Wang, 婧颖 王
Figure caption: The same as the four-parameter case in Figure 21, but with an additional prior of ΩH I ∈ [5 × 10−4, 0.05]. The posterior of ﹩{\bar{M}}_{\mathrm{HI}}﹩ has been converted to ΩH I. The outer, middle, and inner contours denote the 3σ, 2σ, and 1σ regions.
Paper: Emission-line Stacking of 21 cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
Authors: Zhaoting Chen, 兆庭 陈, Steven Cunnington, Alkistis Pourtsidou, Laura Wolz, Marta Spinelli, José Luis Bernal, Matilde Barberi-Squarotti, Stefano Camera, Isabella P. Carucci, José Fonseca, Keith Grainge, Melis O. Irfan, Mario G. Santos, Jingying Wang, 婧颖 王
Figure caption: The same as Figure 21, but with cases of corrected covariance and shuffling covariance for the four-parameter model. From top to bottom, the titles shown are for the shuffling covariance and the corrected covariance, respectively.
Paper: Emission-line Stacking of 21 cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
Authors: Zhaoting Chen, 兆庭 陈, Steven Cunnington, Alkistis Pourtsidou, Laura Wolz, Marta Spinelli, José Luis Bernal, Matilde Barberi-Squarotti, Stefano Camera, Isabella P. Carucci, José Fonseca, Keith Grainge, Melis O. Irfan, Mario G. Santos, Jingying Wang, 婧颖 王
Figure caption: An illustration of the parameterization of the systematics fsys. The black solid line shows the beam ripple. The other three lines show three different sets of parameters for the systematics listed in the figure.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Scanning pattern of the drone over a single array and the resulting maps from this simulated flight. The pattern replicates the programmed flight plan that we have during a typical calibration campaign.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Histogram presenting the uncertainty of the roll angle of the camera estimated using jackknife resampling for each frame. The black vertical line represents the average value of the uncertainty.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: View of the site as seen by the photogrammetry camera. The recognized targets are enclosed in light green squares and a zoom of one of them is presented. Here, we show the process to recognize the target from the image.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Power spectra of a single detector throughout an entire flight for both SO and CLASS. For the SO power spectrum, we highlight both the 8 Hz modulation frequency of the HWP in blue and 47 − 8 Hz and 47 + 8 Hz in gray. Instead, for CLASS the VPM signal is in blue; notice the small lines at 47 − 10 Hz and 47 + 10 Hz that are present here. For both power spectra, we also highlight in black the 47 Hz signal coming from the source.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Parabola fitted to the diffraction pattern. The centroids of all diffraction maxima are plotted as red dots.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Relative position of the pointing of 19 beams in the CRAFTS observation. The 19 beams are rotated by 23﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 for best sampling. The blue circles mark the beam size of ∼3′. In this paper, we add “M” before the beam number to indicate that the data is obtained from the corresponding beam.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: RF schematic output of PROTOCALC. We present also the output power from each components as measured with a power meter. Dashed lines represent coax connections between the components while solid lines represent waveguide connections. Finally, dashed–dotted lines represent communication connections (serial or I2C) between components and the RPi.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Emission of the drone modeled as a blackbody in the 90 GHz band with a bandwidth of 30%, received by a detector in a small aperture-type (like SO-SAT or CLASS) telescope with 50 cm aperture. We included also the power emitted by the PROTOCALC source considering a diffraction-limited single-mode telescope. The vertical dotted line represents the far-field distance, while the horizontal one represents a power of 2 pW, which is a conservative saturation power for transition edge sensor detectors.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: The payload with all the components.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Displacement computed using a thermomechanical simulation on the payload.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Definition of the rotation angle ψ between the camera and the polarization grid. In PROTOCALC, the grid presents a vertical polarization axis, but for visual representation we show a rotated axis to highlight the angle.
Paper: PROTOCALC, a W-band Polarized Calibrator for Cosmic Microwave Background Telescopes: Application to Simons Observatory and CLASS
Authors: Gabriele Coppi, Nadia Dachlythra, Federico Nati, Rolando Dünner-Planella, Alexandre E. Adler, Josquin Errard, Nicholas Galitzki, Yunyang Li, Matthew A. Petroff, Sara M. Simon, Ema Tsang King Sang, Amalia Villarrubia Aguilar, Edward J. Wollack, Mario Zannoni
Figure caption: Error in azimuth and elevation coordinates of the drone at a distance of 500 m and 45° elevation. The typical RTK uncertainty at the Atacama site is 6 cm in the vertical position. The plot shows a worst-case scenario of a constant 10 cm error.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Left: percentage of flagged points at each frequency channel for 5 hr of observation. The blue line shows the result by SumThreshold, and the orange line shows the result from SumThreshold and the SIR algorithm. The gray shadow marks the frequency range (1150–1300 MHz) severely contaminated by RFIs. Right: histogram of the difference (﹩d{ \mathcal D }﹩) between adjacent channels after RFI flagging. The left and right panels show the results for 1050–1150 MHz and 1250–1450 MHz, respectively. The solid lines with different colors represent the histograms of data before RFI flagging (blue), after SumThreshold flagging (orange), and after SumThreshold + SIR flagging (green). The gray dashed lines are Gaussian fit results for RFI-flagged data.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Examples of gt,spec(t) before and after smoothing. The blue line and orange line in each subplot show the gt,spec before and after smoothing, respectively. Top: a normal gt,spec. Middle: gt,spec with an abrupt jump at ∼2.2 hr. Bottom: gt,spec with violent fluctuations.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Left: an example of the comparison of the spectrum at 1 pixel before (blue line in upper panel) and after (red line in upper panel) standing wave removal. Note that the red line has been artificially shifted downward by 15 mJy for clearer comparison. The line in the lower panel shows the difference between the upper two lines. Right: delay spectra of the left upper two spectra. The blue line presents the delay spectrum before standing wave removal, which largely overlaps with the red line, indicating the delay spectrum after standing wave removal. The gray dashed vertical line marks the theoretical position of the peak corresponding to the ∼1.1 MHz standing waves.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Comparison between the flux measured by FAST and the NVSS catalog for 30 sources scanned in Dec+4037_10_05. Blue crosses are for FAST measurement before flux correction. Red circles are with FAST flux after correction. The black line is the y = x line for comparison.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Upper: temporal fluctuations of 19 beams from 1 day’s observation as an example. The temporal variation for each beam has been centered by subtracting the median value over tobs and unmasked frequency channels. Different colors represent different beams. The black thick line is the template baseline. Lower: temporal fluctuations of 19 beams after temporal baseline subtraction. Each colored line represents one beam.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Map-making result for the 5 hr × 5 deg sky area at R.A. from 12 to 17 hr, decl. from ∼40° to ∼45°. This map is the averaged intensity of 1315–1415 MHz.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Left: 〈Vpsr,on(t, ν) − Vpsr,off(t, ν)〉t before (blue line) and after (orange line) smoothing. Right: ﹩{\left\langle \frac{{V}_{{\rm{spec}}}(t,\nu )}{{V}_{{\rm{psr}}}(t,\nu )}\right\rangle }_{t}﹩ before (blue line) and after (orange line) smoothing. The gray shadows in the two plots are the 1150–1300 MHz RFI-contaminated band.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Left: pointing deviation during ∼5 hr of observation for Dec+4142_12_05 on 2022 October 25. The upper panel shows the error of R.A., and the lower panel shows the error of decl. Right: enlargement of the left image at the time range from t ∼ 500 s to t ∼ 600 s.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Waterfall plot of TOD after all calibration and correction processes for ∼5 hr of observation of Dec+4142_12_05, M01, XX polarization. The color represents the temperature, and the blank areas are flagged RFIs.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Left: the upper panel shows a comparison of the percentage of flagged time points at each frequency channel for the all-beam stacked RFI flagging (blue line) and the single-beam flagging on M01 data (red line). The lower panel shows the difference between the upper two lines. The gray shaded area is the severely RFI-contaminated region 1150–1300 MHz that is not included in our scientific analysis. Right: similar to the left image but for the comparison between RFI-flagging results with the single-beam flagging method for M01 (blue line) and M02 (red line), respectively.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: The kurtosis values (upper panel) and skewness values (lower panel) of all 19 beams and two polarizations. The blue lines show values from XX polarization data, and the orange lines are for YY polarization. The black dashed lines represent the mean value μ of kurtosis or skewness of 19 beams and two polarizations, and the red dashed lines show the threshold μ − 3σ that we set to identify bad data.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Percentage of different flagged points at each frequency channel while applying our RFI-flagging algorithm on 19 beam-averaged data and 18 beam-averaged data.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: The average noise diode temperature for each beam at each measurement. The x-axis represents the date of measurement in the format yyyy.m, e.g., “2020.5” means the measurement in 2020 May. Different colored lines with dots show the temperature of different beams.
Paper: CRAFTS for H I Cosmology. I. Data Processing Pipeline and Validation Tests
Authors: Wenxiu Yang, Laura Wolz, Yichao Li, Wenkai Hu, Steven Cunnington, Keith Grainge, Furen Deng, Shifan Zuo, Shuanghao Shu, Xinyang Zhao, Di Li, Zheng Zheng, Marko Krčo, Yinghui Zheng, Linjing Feng, Pei Zuo, Hao Chen, Xue-Jian Jiang, Chen Wang, Pei Wang, Chen-Chen Miao, Yougang Wang, Xuelei Chen
Figure caption: Histograms of the baseline-subtracted g(t). Each subplot represents data from one beam, the blue lines are for XX polarization, and the orange lines are for YY polarization.
Paper: Power-spectrum Space Decomposition of Frequency Tomographic Data for Intensity-mapping Experiments
Authors: Chang Feng, Filipe B. Abdalla
Figure caption: Band powers of mock data at all frequencies arranged in matrices for a single broad band b = 162. The axis is arranged by the indices of all the frequencies {ν} so each subplot is a matrix with all frequencies at a single broad band. The subplot “Mock” is the matrix for the raw band powers of the mock data. The subplot “Residuals,” which is the difference between the “Mock” and the reconstructed foreground, indicates that the H I signals become dominant after the foreground subtraction in power-spectrum space. The subplot “H I (recon)” is the matrix of the reconstructed H I signals, and the subplot “Residuals (H I)” is the difference between the “H I (recon)” and the input H I signals in the auto-power-spectrum subspace.
Paper: Power-spectrum Space Decomposition of Frequency Tomographic Data for Intensity-mapping Experiments
Authors: Chang Feng, Filipe B. Abdalla
Figure caption: (Left) Component power spectra at ν = 980 MHz. The foreground contaminants, including synchrotron emission, free–free emission, anomalous microwave emission, and cosmic microwave background, are a few orders of magnitude brighter than the H I signals, and the H I signals are approximately 2 orders of magnitude stronger than the BAO signals. The absolute values of the BAO component are shown as the dashed lines. (Right) All H I power spectra at frequencies between 925 and 1075 MHz. The BAO components are included in the H I signals. In this work, we ignore redshift distortions and assume that the galaxy bias and H I fraction are constant, i.e., bHI = 1 and ΩHI = 6.2 × 10−4 (E. R. Switzer et al. 2013). For BAO modeling, we adopt the phenomenological model in Equation (7).
Paper: Power-spectrum Space Decomposition of Frequency Tomographic Data for Intensity-mapping Experiments
Authors: Chang Feng, Filipe B. Abdalla
Figure caption: Angular band powers at all frequencies for a single broad band at b = 162. The axis is arranged by the indices of all the frequencies {ν}. The descriptions of “CROSS” and “AUTO” refer to the cross-power-spectrum (×) and auto-power-spectrum subspaces (∘), respectively. The label “FULL” denotes the power-spectrum space without decomposition. The first row shows the power-spectrum space and its decomposition for the overall foreground contamination. The second row corresponds to the H I power spectra. As seen from the last subplot, the H I signal is completely null at the cross-power-spectrum subspace.