adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Top panel: the distribution of the distances of our BHB samples. Bottom panel: the distribution of the relative distance errors.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2 but for the stars with 35∘ < ∣b∣ < 45∘.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2 but for the stars with 45∘ < ∣b∣ < 55∘.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2 but for the stars with 25∘ < ∣b∣ < 35∘.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2 but for the stars with 8∘ < ∣b∣ < 15∘.
Paper: Identification of Blue Horizontal-branch Stars Using Synthetic SkyMapper Colors from Gaia XP Spectra
Authors: Guozhen Hu, Yang Huang, Wenyuan Cui, Tao Wang, Kai Xiao, Ruifeng Shi, Jie Ju, Bowen Huang, Chunyan Li, Zhicun Liu, Xiaolong Wang, Changqing Luo
Figure caption: Similar to Figure 2, but for the stars with 15∘ < ∣b∣ < 25∘.
Paper: A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. I. The “Winged” Radio Galaxies
Authors: Soumen Kumar Bera, Taotao Fang, Tapan K. Sasmal, M. Kunert-Bajraszewska, Xuelei Chen, Soumen Mondal
Figure caption: The images illustrate the improvement in data quality between the LoTSS DR2 (left panel) and the LoTSS DR1 (right panel).
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Top: schematic for MeshBlocks at a refinement boundary. The squares show the active region of each MeshBlock. Bottom: nodal structure inside MeshBlock B. The smaller circles represent the nodes in the MeshBlock, and the larger circles represent the coarse buffers used in AMR communication. The active region is unshaded, and the ghost region is shaded with different gray levels. We also draw schematics for the prolongation and restriction stencils. The smaller yellow circles show the restriction stencil to fill the coarse buffer node highlighted in yellow, and all colored large circles make up the prolongation stencil to fill in the red little circles in the fine ghost zone.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption:  ﹩{L}_{{\rm{rms}}}^{1}﹩ error of linear gravitational wave after one cycle of propagation using different numerical schemes. The red crosses are from runs with a quadrant of the Mesh refined, to test the accuracy for the prolongation and restriction operators described in Section 3.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: AthenaK vs. BAM waveform for a single spinning puncture. Here, we plot the l = 2, m = 0 component of the Weyl scalar extracted at a coordinate radius of 50 M. The difference between the two codes remains small during the course of the evolution.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Mesh refinement structure of a black hole binary with a mass ratio of 20 using the ﹩d\chi -{\rm{\max }}﹩ refinement criterion. The smaller hole automatically receives four more levels of mesh refinement due to its larger gradient in the conformal factor.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Order of convergence from the gauge wave test. The expected orders of convergence are shown as a bold dashed line for the second-order (top), fourth-order (mid), and sixth-order (bottom) algorithms. At high resolution and for high-order differencing, the accumulation of roundoff error quickly dominates and reduces the order of convergence.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Linear wave tests for different initial amplitudes reveal a nonlinear effect. The dashed lines show the expected rate of convergence. Note that the plateau in the rms errors becomes quadratically spaced in the wave amplitude, indicating that they arise from quadratic effects.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Robust stability test at increasing resolution: L2 norm of the Z4c collective constraints (top) and L∞ norm for deviation from flat metric (bottom). Both shown in logarithmic scale.
Paper: Performance-portable Numerical Relativity with AthenaK
Authors: Hengrui Zhu, 恒锐 朱, Jacob Fields, Francesco Zappa, David Radice, James M. Stone, Alireza Rashti, William Cook, Sebastiano Bernuzzi, Boris Daszuta
Figure caption: Constraint violation monitoring for the gauge wave test. The spatial differencing algorithms are labeled by the number of ghost points Ng, and the dashed lines correspond to runs with twice the resolution. As expected, the error decreases drastically with the order of the spatial algorithms and with the resolution.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: Left: a diagram of the FB2 optical design showing the light path through the telescope and instrument, beginning with the siderostat. A calibration system cap is mounted to the top of the instrument housing, where a shutter opens to allow light from the telescope into the instrument. Right: a detailed CAD rendering of the FB2 spectrograph, including a two-mirror FC, mask-guider system with visible-light guider camera, two spherical mirror pairs with two folding flats (FFs), a diffraction grating, and an EMCCD. The spectrograph is housed in a vacuum chamber that sits below the large optics. Figure from V. Picouet et al. (2020).
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Timing diagram of radial velocity Vr (km s−1, left), proton number density (105 cm−3 at 3 Rs and 103 cm−3 at 20 Rs, middle), and decadic logarithms of plasma β (top right) and radial magnetic field polarities (bottom right) with “−1” denoting the field pointing to the Sun and “1” for the field directed away from the Sun, as observed by a virtual satellite located at 3 Rs (top) and 20 Rs (bottom), positioned at 60° behind Earth in longitude and at the same latitude. The black solid lines and black square symbols represent the simulated variables, while the gray solid lines indicate the variables derived from Wind satellite observations, which have been mapped from 1 au to 20 Rs following the ballistic propagation.
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Synoptic maps of east-limb white-light pB images at 3 Rs observed by the LASCO-C2 instrument on board the SOHO satellite (top) for CRs 2110 (left) and 2111 (right), alongside the timing diagrams of simulated plasma number density (105 cm−3) and radial velocity Vr (km s−1 at 3 Rs at the east-limb longitude of the Sun in the Earth view.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: Top: a schematic diagram of the FB2 FC alignment scheme. The inner portion of the CGH and four “spokes” serve as an alignment pattern to orient the CGH relative to the interferometer, and annuli at larger radii serve as nulling patterns for the FC1 (inner-pattern) and FC2 (outer-pattern) optics. Bottom: the FB2 FC alignment setup. An interferometer is placed at image left, and the CGH is between the two FC mirrors. Each FC optic is mechanically constrained with alignment apparatus and supported by stage stacks allowing motion in x, y, z, tip, and tilt. The left panel of the monitor in the background shows the interferometer alignment pattern of the CGH, including the central, circular portion and the four radial spokes, and the right panel shows the wrapped phase map for a region of the alignment pattern.
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: White-light pB images observed by COR2/STEREO-A (top), ranging from 2.5 Rs to 15 Rs, alongside corresponding pB images synthesized from simulation results ranging from 2.5 Rs to 15 Rs (middle) and 2D distributions of some selected simulated magnetic field lines from 1 Rs to 6 Rs (bottom). These images are shown on the meridional plane in the STEREO-A view.
Paper: SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
Authors: Haopeng Wang, Liping Yang, Stefaan Poedts, Andrea Lani, Yuhao Zhou, Yuhang Gao, Luis Linan, Jiakun Lv, Tinatin Baratashvili, Jinhan Guo, Rong Lin, Zhan Su, Caixia Li, Man Zhang, Wenwen Wei, Yun Yang, Yucong Li, Xinyi Ma, Edin Husidic, Hyun-Jin Jeong, Mahdi Najafi-Ziyazi, Juan Wang, Brigitte Schmieder
Figure caption: Timing diagrams of simulated plasma number density (103 cm−3, top), radial velocity Vr (km s−1, middle) and temperature (105 K, bottom) at 20 Rs, corresponding to the same longitude as in Figure 7.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: The FB2 gondola mechanical structure, with doors open. The 1 m primary mirror is integrated into the gondola upper structure, and the 1.2 m siderostat is affixed on support frames near the center of the gondola. In the lower bay, the instrument and all support equipment are mounted prior to flight.
Paper: The 2023 Flight of the Faint Intergalactic-medium Redshifted Emission Balloon
Authors: Drew M. Miles, Vincent Picouet, Zeren Lin, Ignacio Cevallos-Aleman, David Schiminovich, Nicolas Bray, Charles-Antoine Chevrier, Greyson Davis, Erika Hamden, Keri Hoadley, D. Christopher Martin, Bruno Milliard, Johan Montel, David Valls-Gabaud, Simran Agarwal, Philippe Balard, Patrick Blanchard, Harrison Bradley, Haeun Chung, Marty Crabill, Fernando Cruz Aguirre, Xihan Deng, Fabien Harmand, Catherine Hourtolle, Olivia Jones, Nazende I. Kerkeser, Aafaque R. Khan, Gillian Kyne, Jessica S. Li, Nicole Melso, Shouleh Nikzad, Julie Richard, Meghna Sitaram, Jared Termini, Jean-Noel Valdivia, Didier Vibert, Matthew Werneken
Figure caption: A transparent CAD representation of the FB2 instrument with new or modified baffles emphasized in solid color, from T. Brendel et al. (2022).
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: Schematic of the frequency-comb-calibrated LHR system currently in operation at NIST Boulder. Panel (a) shows the rooftop-mounted solar tracker, and panel (b) highlights the fiber-coupling optics mounted to the solar tracker. Panel (c) shows the fiber optic configuration and RF power detection circuit (green box) used to measure the 1565 nm solar Fe I transition and frequency calibration “ticks” as the LO laser is scanned across the solar transition (panel (d)). Light from an additional reference laser locked to the frequency comb generates an additional pair of “reference ticks” that are used to determine the absolute frequency of the measured spectrum. The frequency comb is referenced to an NIST-calibrated hydrogen maser that is directly traceable to the SI second. All components in panel (c) are located in a rooftop laboratory adjacent to the solar tracker. OFC: optical frequency comb; WDM: wavelength division multiplexer; VOA: variable optical attenuator; SMF: single-mode optical fiber; PMF: polarization-maintaining optical fiber; BPD: balanced photodetector; LPF: low-pass filter; Amp: amplifier; Split: power splitter; Mix: RF mixer.
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: RVs measured using the comb-calibrated LHR system from 2023 September 21 to November 5. Panel (a) shows the individual RV measurements (blue points) and the daily average RV (orange points) for each day. Panel (b) highlights the daily average RV measurements, which indicate a slow drift by ∼310 kHz day−1. Panels (c) and (d) show the RV measurements for a representative day (2023 September 28) and corresponding Allan deviation showing the frequency precision of our measurements before (gray) and after (green) detrending to correct for the pointing-induced diurnal drift. Error bars are shown for every 150 measurements for clarity. Panels (e) and (f) show RV measurements for 2023 October 17. All times are specified in UTC. All error bars are calculated using the methods described in Section 4.
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: Measured solar spectrum from 2023 October 7. The optical frequency is specified relative to 191.52759375(4) THz. The blue curve shows a single 5 s measurement, while the orange curve shows the spectrum after averaging over the full day. The green curve shows the line bisector determined from the averaged spectrum. Telluric lines have been subtracted using the procedure described in Section 4.6, and the vertical dashed line indicates the expected position of the Fe I line specified by the VALD3 database (R. C. Peterson & R. L. Kurucz 2014; T. Ryabchikova et al. 2015).
Paper: Frequency-comb-calibrated Laser Heterodyne Radiometry for Precision Radial Velocity Measurements
Authors: Ryan K. Cole, Connor Fredrick, Winter Parts, Max Kingston, Carolyn Chinatti, Josiah Tusler, Suvrath Mahadevan, Ryan Terrien, Scott A. Diddams
Figure caption: The LHR antenna pattern imaged with a beam profiler. Panel (a) shows the antenna pattern measured before the start of the 6-week data set, along with horizontal and vertical cross sections measured along the center line. Panel (b) shows the pattern measured after 6 weeks of continuous observations. Comparison of the cross sections measured before data collection (blue) and after (red) shows a clear asymmetry that has developed owing to relaxation of the fiber-coupling optics.
Paper: Polarization Characteristics of the Hyperactive FRB 20240114A
Authors: Jin-Tao Xie, Yi Feng, Di Li, Yong-Kun Zhang, Deng-Ke Zhou, Yuanhong Qu, Xiang-han Cui, Jian-Hua Fang, Jia-Ying Xu, Chen-Chen Miao, Mao Yuan, Chao-Wei Tsai, Pei Wang, Chen-Hui Niu, Xianglei Chen, Mengyao Xue, Junshuo Zhang
Figure caption: Two examples of calculated frequency burst ranges, both originating from FRB 20220912A (Y.-K. Zhang et al. 2023). In the upper panel, the black solid line represents the spectrum of the burst, the green dashed line denotes the CDF of the spectrum, and the red solid line indicates the smoothed CDF after filtering.
Paper: Polarization Characteristics of the Hyperactive FRB 20240114A
Authors: Jin-Tao Xie, Yi Feng, Di Li, Yong-Kun Zhang, Deng-Ke Zhou, Yuanhong Qu, Xiang-han Cui, Jian-Hua Fang, Jia-Ying Xu, Chen-Chen Miao, Mao Yuan, Chao-Wei Tsai, Pei Wang, Chen-Hui Niu, Xianglei Chen, Mengyao Xue, Junshuo Zhang
Figure caption: (A) Histograms of linear polarization fraction L/I for FRB 20240114A, FRB 20220912A, and FRB 20201124A. (B) Correlations between linear polarization fraction L/I and circular polarization fraction V/I for FRB 20240114A, FRB 20220912A, and FRB 20201124A. The gray dashed semicircles denote the areas in which the degree of polarization ﹩P/I=\sqrt{{L}^{2}+{V}^{2}}/I\leqslant 1﹩. The gray sectors cover 68% of bursts from FRB 20240114A. (C) Histograms of circular polarization fraction V/I for FRB 20240114A, FRB 20220912A, and FRB 20201124A.
Paper: Polarization Characteristics of the Hyperactive FRB 20240114A
Authors: Jin-Tao Xie, Yi Feng, Di Li, Yong-Kun Zhang, Deng-Ke Zhou, Yuanhong Qu, Xiang-han Cui, Jian-Hua Fang, Jia-Ying Xu, Chen-Chen Miao, Mao Yuan, Chao-Wei Tsai, Pei Wang, Chen-Hui Niu, Xianglei Chen, Mengyao Xue, Junshuo Zhang
Figure caption: Polarization position angle and intensity profiles, along with dynamic spectra, for four bursts from FRB 20240114A. In each panel: subpanel (A) displays the polarization position angles; subpanel (B) presents the burst profiles, with lines representing total intensity (black, normalized to a peak value of 1.0), linear polarization (red), and circular polarization (blue); subpanel (C) shows the dynamic spectra.
Paper: Polarization Characteristics of the Hyperactive FRB 20240114A
Authors: Jin-Tao Xie, Yi Feng, Di Li, Yong-Kun Zhang, Deng-Ke Zhou, Yuanhong Qu, Xiang-han Cui, Jian-Hua Fang, Jia-Ying Xu, Chen-Chen Miao, Mao Yuan, Chao-Wei Tsai, Pei Wang, Chen-Hui Niu, Xianglei Chen, Mengyao Xue, Junshuo Zhang
Figure caption: Waiting time distribution of FRB 20240114A. The blue step plot represents the distribution of waiting times, while the red curve denotes the fit using two log-normal components.
Paper: Polarization Characteristics of the Hyperactive FRB 20240114A
Authors: Jin-Tao Xie, Yi Feng, Di Li, Yong-Kun Zhang, Deng-Ke Zhou, Yuanhong Qu, Xiang-han Cui, Jian-Hua Fang, Jia-Ying Xu, Chen-Chen Miao, Mao Yuan, Chao-Wei Tsai, Pei Wang, Chen-Hui Niu, Xianglei Chen, Mengyao Xue, Junshuo Zhang
Figure caption: Histograms of specific fluence for FRB 20240114A. The red line represents the kernel density estimation (KDE) of the specific fluence distribution.
Paper: High-efficiency and Low-noise Detectors for the Upgraded CLASS 90 GHz Focal Plane
Authors: Carolina Núñez, John W. Appel, Rahul Datta, Charles L. Bennett, Michael K. Brewer, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Nicholas Costen, Jullianna Denes Couto, Sumit Dahal, Kevin L. Denis, Joseph R. Eimer, Thomas Essinger-Hileman, Jeffrey Iuliano, Yunyang Li, Tobias A. Marriage, Jennette Mateo, Matthew A. Petroff, Rui Shi, Karwan Rostem, Deniz A. N. Valle, Duncan Watts, Edward J. Wollack, Lingzhen Zeng
Figure caption: Distributions of TES electrothermal parameters relative to their per wafer median value: thermal conductance (G), prefactor (κ), saturation power for Tbath = 50 mK (Psat), normal resistance (RN), critical temperature (Tc), thermal time constant (τ), optical time constant (τγ), and heat capacity (C). Estimation of these parameters is described in Section 4. Outliers beyond 3σ from the per wafer median of the underlying distributions have been excluded. Subplot titles show the standard deviation of the histograms. Per wafer median values for all parameters are given in Table 1. These distributions can be compared to previously published results for the original W-band array (Figure 7 in S. Dahal et al. 2018) and the Q-band array (Figure 4 in J. W. Appel et al. 2014). The TES parameters in the upgraded W-band wafers show greater uniformity than those in the original wafers but do not match the consistency achieved by selecting individual pixels from Q-band wafers.