adsabs/AstroCLIMB huggingface dataset:
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The CSPFB structure.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The second polyphase decomposition structure of the kth polyphase branch in a fractional overlap OPFB.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The OPFB structure after the first polyphase decomposition. Here “first” refers to the first polyphase decomposition of the dual decomposition method for convenience in the subsequent discussion.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The subband passband of the OPFB. Both subband edge attenuation and spectral aliasing occur in the overlapping regions between subbands.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The successive loading of data samples and serpentine movement of data through the 2D polyphase filter for M/D = 6/4 proposed by J. Tuthill et al. (2015) and J. P. Smith et al. (2021).
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The problems of the CSPFB. Signal amplitude attenuation and spectral aliasing occur at the subband boundaries, resulting in the degradation of useful information.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The OPFB structure for the integer M/D.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The dynamic spectrum synthesized from six subbands: (a) J1935+1616, (b) J2022+2854, and (c) J2022+5154.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The dynamic spectrum of J0332+5434 synthesized from six subbands.
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: The top left and right panels show the distribution of the training set in the plane of (BP − RP)0–[Fe/H] and (BP − RP)0–MG, respectively. The bottom three panels each compares eight representative Gaia XP spectra from the training set that spans a range of [Fe/H] values but share similar (BP − RP)0 colors of approximately 0.85, 1.15, and 1.55, respectively. The dots in the top right panel and the lines in the bottom three panels are color coded by [Fe/H].
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: (a) Histogram of the residuals Δ[Fe/H], with the mean and standard deviation values labeled. (b) Comparison of [Fe/H] values for common stars between our results and the PASTEL catalog. The red solid line is the one-to-one line. (c)–(f) Fitting residuals as a function of [Fe/H], intrinsic BP − RP color, G magnitude, and E(B − V). The red and blue solid lines indicate the mean deviation and 1σ uncertainties, respectively. (g) The color–magnitude diagram, color coded by Δ[Fe/H]. (h) The distribution of the predicted [Fe/H] of the training set in the plane of (BP − RP)0–MG, color coded by [Fe/H] values from our model.
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: Similar to Figure 3 but for the SAGA catalog.
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: Comparisons between typical predicted errors (y-axis) from the UA-CSNet and 1σ uncertainties of the residuals (x-axis) for the PASTEL (left panel) and SAGA (right panel) catalogs in different G-magnitude bins.
Paper: Metallicities of 20 Million Giant Stars Based on Gaia XP Spectra
Authors: Lin Yang, 琳 杨, Haibo Yuan, 海波 苑, Bowen Huang, 博闻 黄, Ruoyi Zhang, 若羿 张, Timothy C. Beers, Kai Xiao, 凯 肖, Shuai Xu, 帅 徐, Yang Huang, 样 黄, Maosheng Xiang, 茂盛 向, Meng Zhang, 萌 张, Jinming Zhang, 津铭 张
Figure caption: The structure of the proposed UA-CSNet.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Phase-folded I-band light curves of the prototype object OGLE-BLAP-001 and 36 BLAPs detected by the OGLE survey toward the Galactic bulge. For the majority of the bulge objects, all available OGLE-IV time-series data (from years 2010–2019) are presented, whereas for several objects only part of the data was selected to clearly show the light-curve shape (e.g., OGLE-BLAP-030). The most characteristic feature in BLAPs is the sharp maximum. An additional bump is seen in objects with periods exceeding 40 minutes.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Period vs. I-band amplitude diagram for BLAPs observed toward the Galactic bulge. The diagram also includes the prototype object from the Galactic disk. Open dots refer to objects with an additional bump in the light curve.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Location of the BLAPs in the atmospheric parameter spaces. The 15 stars included in this work are indicated with red symbols and OGLE-BLAP-030 (multimode pulsator) is indicated with an additional black circle. The four high-gravity BLAPs of T. Kupfer et al. (2019) are plotted in blue. The gray symbols are for the two BLAPs with low-resolution spectra analyzed in P. Pietrukowicz et al. (2017), and the green symbols are for TMTS-BLAP-1, OGLE-BLAP-009, and SMSS-BLAP-1 (J. Lin et al. 2023; C. W. Bradshaw et al. 2024; S.-W. Chang et al. 2024). Open squares indicate BLAPs with a He-poor atmosphere and filled circles BLAPs with a He-rich atmosphere. The evolutionary tracks for low-mass He-core pre-WDs are from T. Kupfer et al. (2019).
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Variations of the pulsation signal in the multimode object OGLE-BLAP-030. The OGLE-IV data are divided into seasons from 2010 to 2019. The left column shows, for each of the seasons, the I-band light curve phased with the dominant period. The magnitude range on the vertical axis is the same in each subpanel. The right column shows the power spectrum obtained after subtraction of the actual dominant period. Period and amplitude changes over the years are presented in the bottom panel. Period uncertainties are smaller than the dots.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Best fit to the spectra of two He-poor BLAPs in our spectroscopic sample: OGLE-BLAP-037 (= OW J1819-2729) and OGLE-BLAP-044 (J. Borowicz et al. 2023).
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: O − C diagrams constructed for six selected BLAPs observed in OGLE-III and OGLE-IV over years 2001–2019. Objects OGLE-BLAP-007 and OGLE-BLAP-022 show evident negative and positive period changes, respectively. Changes in the remaining objects are irregular.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Moderate-resolution spectra of six selected BLAPs. The best-fit synthetic spectra are shown with red lines. The interstellar Na I D lines are cut out for some of the spectra during the fitting procedure. The obtained atmospheric parameters as well as the pulsation period are provided for each object. Very similar parameters indicate that the stars form a homogeneous group of objects.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: O − C diagrams constructed for four BLAPs observed during three phases of the OGLE project, from OGLE-II to OGLE-IV covering years 1997–2019. The differences measured in OGLE-BLAP-019 indicate positive period changes in this pulsator.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Spectroscopic lines identified in He-rich BLAPs. The spectrum is a combination of the RV-corrected spectra of OGLE-BLAP-010, 019, 021, 031, and 034. The ion and wavelength (in angstroms) of the strongest transitions are marked.
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Synthetic spectra with solar (blue line) and supersolar abundances (red line) compared to the spectra of OGLE-BLAP-031 (top) and OGLE-BLAP-010 (bottom).
Paper: Observational Parameters of Blue Large-amplitude Pulsators 
Authors: Paweł Pietrukowicz, Marilyn Latour, Igor Soszyński, Francesco Di Mille, Piera Soto King, Rodolfo Angeloni, Radosław Poleski, Andrzej Udalski, Michał K. Szymański, Krzysztof Ulaczyk, Szymon Kozłowski, Jan Skowron, Dorota M. Skowron, Przemek Mróz, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Period change rates for BLAPs observed in OGLE-III and OGLE-IV. The rates were calculated based on the period values determined for each phase (Equation (1)).
Paper: A Full Active Galactic Nuclei Feedback Prescription for Numerical Models: Negative, Positive, and Hot Gas-ejection Modes
Authors: Emanuele Contini, Sukyoung K. Yi, Jinsu Rhee, Seyoung Jeon
Figure caption: The star formation history of four sample galaxies (top four panels), ordered by increasing stellar mass from top to bottom, from redshift z ∼ 10 to the present time. The green line represents the secular evolution, the blue line indicates the SFR due solely to positive AGN feedback, while the red one represents the total SFR (shifted 0.1 dex upward for easier viewing). Several interesting features can be observed in these plots. From top to bottom, it is clear that the contribution of positive AGN feedback to the total SFR increases, as expected from Figure 5. This trend is evident not only in terms of the mass provided but also in the duration of activity of the positive feedback mode. Specifically, in lower-mass galaxies, the contribution is shorter and characterized by episodic bursts, whereas in higher-mass galaxies, the SFR history driven by the positive AGN feedback more closely follows the total SFR, being continuous rather than broken or irregular, and being longer and more sustained. In all cases, the positive feedback mode is efficient at high redshift and begins to fade as the negative feedback mode takes over the cooling process, indicating that the negative mode reaches its peak power. The two bottom panels show, instead, the distributions (median, and 16th and 84th percentiles) of the SFR histories for wide samples of galaxies in the stellar mass ranges ﹩10.5\lt {\rm{log}}\,({M}_{\ast }/{M}_{\odot })\lt 11.5﹩ (bottom left panel) and ﹩{\rm{log}}\,({M}_{\ast }/{M}_{\odot })\gt 11.5﹩ (bottom right panel).
Paper: A Full Active Galactic Nuclei Feedback Prescription for Numerical Models: Negative, Positive, and Hot Gas-ejection Modes
Authors: Emanuele Contini, Sukyoung K. Yi, Jinsu Rhee, Seyoung Jeon
Figure caption: The fraction of mass for different components (stars, cold gas, hot gas, and ejected gas) within the virial radius, normalized by the universal baryon fraction, as a function of halo mass. Different colors represent the various components, and the dashed and solid lines distinguish the predictions from FEGA24 and FEGA25, respectively. Our models are compared with the observed hot gas fraction from P. Popesso et al. (2024; magenta diamonds with error bars) and a set of observed hot gas fractions from various authors (A. Vikhlinin et al. 2006; M. Arnaud et al. 2007; G. W. Pratt et al. 2009; J. Rasmussen & T. J. Ponman 2009; M. Sun et al. 2009; A. H. Gonzalez et al. 2013; A. Mahdavi et al. 2013; L. Lovisari et al. 2015; D. Eckert et al. 2016, 2019; R. J. Pearson et al. 2017; S. L. Mulroy et al. 2019; A. Ragagnin et al. 2022; dark blue circles). Given the importance of sampling halos down to ﹩{\rm{log}}\,({M}_{{\rm{halo}}}/{M}_{\odot })=11﹩, for this plot we also make use of the catalogs obtained by running the models on the merger trees extracted from YS50HR. It is important to note that, despite the large scatter in the observed data, FEGA24 fails to predict a reasonable hot gas fraction for halos smaller than large groups (﹩{\rm{log}}\,({M}_{{\rm{halo}}}/{M}_{\odot })\lt 14﹩). In contrast, FEGA25, with its new hot gas ejection mode in AGN feedback, performs significantly better. This result underscores the importance of having a mechanism, such as the hot gas ejection mode, that can expel gas from the halo without significantly altering the cold gas and stellar mass content.
Paper: Simons Observatory: Characterization of the Large Aperture Telescope Receiver
Authors: Tanay Bhandarkar, Saianeesh K. Haridas, Jeff Iuliano, Anna Kofman, Alex Manduca, Karen Perez Sarmiento, John Orlowski-Scherer, Thomas P. Satterthwaite, Yuhan Wang, Zeeshan Ahmed, Jason E. Austermann, Kyuyoung Bae, Gabriele Coppi, Mark J. Devlin, Simon R Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Jon E. Gudmundsson, Shawn W. Henderson, Johannes Hubmayr, Bradley R. Johnson, Matthew A. Koc, Brian J. Koopman, Michele Limon, Michael J Link, Tammy J. Lucas, Jenna E. Moore, Federico Nati, Michael D. Niemack, Carlos E. Sierra, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Suzanne T. Staggs, Robert J. Thornton, Tran Tsan, Jeff L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Mario Zannoni, Kaiwen Zheng
Figure caption: Left panel: the temperature of LATR cold stages during constant-elevation LAT scans and slewing between azimuth locations at that elevation, divided by their median during this period (upper plot) and the telescope’s azimuth (lower plot). The slew occurs at ∼800 s and has a speed of 4° s−1 with starting and ending accelerations of 4° s−2. All lines except the “UFM” one were measured by a single thermometer at each of the DR cold stages; the“UFM” line was measured at one representative array. We see a subpercent-level temperature change on these cold stages, which is well within the specifications mentioned in Section 2.4. Most of the noise seen in the 4 K and 100 mK stage can be attributed to readout noise. Slewing and scanning periods are both included because their respective parameters differ; see the text for more information. Right panel: temperatures at the UFM, binned over five constant-elevation scans (10 total throws) from 30°–150° that begin at ∼1000 s into the scans featured in the plot on the left. The dotted black vertical lines indicate the azimuth angles for which turnarounds occur, and the green solid line is a line of best fit, with a linear correlation coefficient of r = −0.100. We find the peak-to-peak temperature swings to be ∼0.25 mK or less.
Paper: Simons Observatory: Characterization of the Large Aperture Telescope Receiver
Authors: Tanay Bhandarkar, Saianeesh K. Haridas, Jeff Iuliano, Anna Kofman, Alex Manduca, Karen Perez Sarmiento, John Orlowski-Scherer, Thomas P. Satterthwaite, Yuhan Wang, Zeeshan Ahmed, Jason E. Austermann, Kyuyoung Bae, Gabriele Coppi, Mark J. Devlin, Simon R Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Jon E. Gudmundsson, Shawn W. Henderson, Johannes Hubmayr, Bradley R. Johnson, Matthew A. Koc, Brian J. Koopman, Michele Limon, Michael J Link, Tammy J. Lucas, Jenna E. Moore, Federico Nati, Michael D. Niemack, Carlos E. Sierra, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Suzanne T. Staggs, Robert J. Thornton, Tran Tsan, Jeff L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Mario Zannoni, Kaiwen Zheng
Figure caption: The auto-spectral density (ASD) of all detectors in the dark configuration before and after common-mode subtraction. The solid line is the median of all detectors when scanning, and the dashed line is the median of all detectors when staring. The contour is the 1σ level of these distributions. Blue is the 90 GHz detectors, and red is the 150 GHz detectors. Note that the solid and dashed lines sit on top of or very close to each other across the entire frequency range. The spikes in the ASD before removing the common mode are mostly sourced from an issue with a single UFM. The remaining bumps after common-mode subtraction are 50 Hz (AC power), 1.4 Hz (pulse tube operating frequency), and 2.8 Hz (harmonic of the 1.4 Hz bump) and coupled to the detectors in complex ways that are not completely common mode. The inset plot on Figure 11(a) shows the ASD in the frequency range of our turnarounds, with the black vertical line being the turnaround frequency (0.008 Hz). This figure modified from that in S. K. Haridas et al. (2024).
Paper: Simons Observatory: Characterization of the Large Aperture Telescope Receiver
Authors: Tanay Bhandarkar, Saianeesh K. Haridas, Jeff Iuliano, Anna Kofman, Alex Manduca, Karen Perez Sarmiento, John Orlowski-Scherer, Thomas P. Satterthwaite, Yuhan Wang, Zeeshan Ahmed, Jason E. Austermann, Kyuyoung Bae, Gabriele Coppi, Mark J. Devlin, Simon R Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Jon E. Gudmundsson, Shawn W. Henderson, Johannes Hubmayr, Bradley R. Johnson, Matthew A. Koc, Brian J. Koopman, Michele Limon, Michael J Link, Tammy J. Lucas, Jenna E. Moore, Federico Nati, Michael D. Niemack, Carlos E. Sierra, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Suzanne T. Staggs, Robert J. Thornton, Tran Tsan, Jeff L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Mario Zannoni, Kaiwen Zheng
Figure caption: White noise levels of our time-ordered data (TODs) with OTs capped at 4 K, including data of all detectors in the dark configuration. The solid line indicates when scanning, and the dashed indicates when staring. Blue is the 90 GHz detectors, and red is the 150 GHz detectors. The predicted bands are the expected noise for the dark configuration from BoloCalc, spanning the range from the goal and baseline configurations. Figure from S. K. Haridas et al. (2024).
Paper: Simons Observatory: Characterization of the Large Aperture Telescope Receiver
Authors: Tanay Bhandarkar, Saianeesh K. Haridas, Jeff Iuliano, Anna Kofman, Alex Manduca, Karen Perez Sarmiento, John Orlowski-Scherer, Thomas P. Satterthwaite, Yuhan Wang, Zeeshan Ahmed, Jason E. Austermann, Kyuyoung Bae, Gabriele Coppi, Mark J. Devlin, Simon R Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Jon E. Gudmundsson, Shawn W. Henderson, Johannes Hubmayr, Bradley R. Johnson, Matthew A. Koc, Brian J. Koopman, Michele Limon, Michael J Link, Tammy J. Lucas, Jenna E. Moore, Federico Nati, Michael D. Niemack, Carlos E. Sierra, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Suzanne T. Staggs, Robert J. Thornton, Tran Tsan, Jeff L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Mario Zannoni, Kaiwen Zheng
Figure caption: A photo of the LAT at the Chilean site, as of 2024 March. In this image, the receiver cabin is located toward the top left of the structure.
Paper: A Dual Polyphase Decomposition Overlapped Polyphase Filter Bank and Its Implementation in a Field-programmable Gate Array
Authors: Shaocong Guo, Qiao Meng, Hailong Zhang, Yazhou Zhang, Chenye Zhou, Gaojing Li, Jie Wu, Jianxun Shao
Figure caption: The configuration interface of the interpolated FIR IP core within Vivado when m = 2.