adsabs/AstroCLIMB huggingface dataset:
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Phase-folded light curve of the OGLE-LMC-HB-0287 (top panel). The light curve is a combination of the heartbeat variation with an orbital period, Porb = 274.93 days (middle panel) and dimmings, which are probably caused by a dark spot on the primary’s surface, with a rotational period, Prot = Porb/3 = 91.64 days (bottom panel). In the middle panel, we present the light curve from the top panel after subtracting the dimming caused by the spot. With the red line we plot the fitted Kumar et al.’s model. In the bottom panel, we show a phase-folded light curve with Prot after subtracting the heartbeat variation. With green dots we mark the median I−band magnitude in the 0.1 phase bins. Green bars represent a standard deviation of the magnitude in the bin.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Examples of time-domain (left panels) and phase-folded light curves (right panels) of HBSs exhibiting OSARG pulsations. Colors of the points denote the observation time. The color scale is the same in all panels.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Phase-folded light curves of the sample of HBSs exhibiting high-amplitude TEOs. The TEOs are visible as oscillations outside periastron.
Paper: The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Marcin Wrona, Milena Ratajczak, Piotr A. Kołaczek-Szymański, Szymon Kozłowski, Igor Soszyński, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Paweł Pietrukowicz, Dorota M. Skowron, Jan Skowron, Przemek Mróz, Radosław Poleski, Mariusz Gromadzki, Krzysztof Ulaczyk, and Krzysztof Rybicki
Figure caption: Light curves of two HBSs showing unusual brightness variations. Time-domain (left panel) and phase-folded light curves (right panel) are presented. We marked the first and last three observational seasons with red and blue colors, respectively.
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: Upper panel: power spectrum measurements at redshift z = 0 and z = 1. Predictions from the Cosmic Emulator by Heitmann et al. (2014) are shown for comparison. Lower panels: ratio of the simulation and the emulator at both redshifts out to k = 10h Mpc−1, the maximum range for which the emulator was developed. The light blue bands indicate a 5% range. The results are within the accuracy bounds reported in Heitmann et al. (2014).
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: Visualization of the particle light cone data out to z = 0.6 (upper panels) and a zoom-in to z = 0.15 (lower panels). The orange curve in the upper panels shows the z = 0.15 boundary. The color in the upper panels represents depth in the disk of particles (in Mpc h−1). In the lower panels, color represents LOS velocities (in comoving km s−1). The left panels render the comoving particle positions while the right panels demonstrate the so-called Fingers of God effect from redshift space distortion.
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: Upper panel: Farpoint halo mass function measurements at redshifts z = 0 and z = 1. We compare the results to the mass function emulator of Bocquet et al. (2020). Middle and lower panels: ratio of the simulation and the emulator results at both redshifts. Note that the emulator only provides predictions down to M200c ∼ 1013h−1 M⊙. For the mass range covered, the agreement is excellent and within the accuracy bounds reported in Bocquet et al. (2020).
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: Measurement of the halo concentration–mass relation at redshifts z = 0 (purple) and z = 1 (light blue). The shaded region shows the 1σ standard deviation for z = 0. For comparison, we show the fitting function derived in Child et al. (2018) as implemented in the COLOSSUS package (Diemer 2018). For the very low-mass regime, the fit is represented by a dashed line, indicating that the results from Child et al. (2018) were extrapolated in this mass range.
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: The Farpoint particle correlation function at z = 0. The measurement from the simulation is shown in purple and predictions from the Mira–Titan emulator described in Lawrence et al. (2017) are shown in light blue. The BAO peak is visible at the right edge of the image. The ample resolution of the simulation allows us to evaluate the correlation function to scales down to 0.1h−1 Mpc.
Paper: Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Nicholas Frontiere, Katrin Heitmann, Esteban Rangel, Patricia Larsen, Adrian Pope, Imran Sultan, Thomas Uram, Salman Habib, Silvio Rizzi, and Joe Insley
Figure caption: Results from the application of the SMACC approach to the Farpoint simulation. Upper panels: average core mass functions at z = 0 (left) and z = 1 (right) for five host halo mass bins. (Details of the host mass bins are listed in Table 2.) Points for which ﹩\mathrm{log}(m/M)\leqslant \mathrm{log}(100{m}_{p,\mathrm{FP}}/\langle M\rangle )﹩ have enhanced color transparency, where mp,FP is the particle mass of the Farpoint simulation and 〈M〉 is the average host halo mass of each host halo bin. Following Sultan et al. (2021), for each host halo mass bin we fit Equation (9) to the opaque data points with α fixed to 0.94 and 0.8 for z = 0 and z = 1, and allow AM to vary. Lower panels: ratio of the opaque points of the core mass function (shown in the upper panel) to the fitting function, for each host halo mass bin and redshift. The best-fit parameter value for AM is indicated in each panel.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The schematic diagram of the timing system of Insight-HXMT. The GPS receiver (GPSR) sends the GPS pulse per second (PPS) to the electronic boxes of the three payloads. The high-stability time unit (HSTU) on the platform distributes 5 MHz clocks to HE and LE. The clock distributor in HE uses the 5 MHz clocks to generate a local clock with a period of 2 μs for the data processing unit (DPU) of HE. The clock distributor in LE also utilizes the 5 MHz clock to generate the local clock with a period of 1 μs and sends it to DPU. ME uses a quartz oscillator instead to generate a 6 μs clock to DPU.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The time assignment of Insight-HXMT/HE events. GPS events recorded by Stime and Ptime are shown with a big solid circle and inserted into the event stream every second. The physical events with a small solid circle are only recorded by Ptime. Ptime accumulates to 219 and starts counting from zero.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The evolution trends of the relative change of the nominal period for HE and LE. The blue line represents the result of LE, and the green line represents the result of HE. Reasons for the deviations from the long time trend around day 200 are yet unknown.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: (a) The top panel shows the evolution of the relative change of the nominal period for ME. The bottom panel shows the temperature vs. days after launch. The real period of the quartz oscillation depends largely on temperature. (b) The correlation between temperature and the relative change of the nominal period R.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The residuals between the arrival time of the GPS pulse in 1 hr calculated by Equation (1) and Stime, which is an integer in seconds. The top panel shows the residual for HE, and the residual is less than 2 μs, which is the period of the local clock. The bottom panel shows the residual for LE, and the residual is less than 1 μs, which is the period of the local clock. The slope of each truncated line in each panel refers to the R in Figure 3.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The residuals between the arrival time of GPS pulse in 1 hr calculated by Equation (1) and Stime for ME. Panel (a) shows the residual using S0, τ, and ﹩\dot{\tau }﹩. Panel (b) shows the residual using S0 ,τ, ﹩\dot{\tau }﹩ and ﹩\ddot{\tau }﹩. Panel (c) shows the residual using S0, τ, ﹩\dot{\tau }﹩, ﹩\ddot{\tau }﹩, and ﹩\dddot{\tau }﹩.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The top panel and the bottom panel show the relation between the ToA errors and the exposure time of the corresponding profiles for HE and ME, respectively. The errors of the ToAs calculated from the signal-to-noise ratios of the main peak are presented as squares, and the errors in the ToA fits are plotted as triangles. The red lines indicate the linear relation to the square root of the exposure time.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The pulse profile of the Crab pulsar observed by Insight-HXMT in three energy bands, using the Jodrell Bank Crab ephemeris. The red, blue, and black lines indicate the profiles of the three payloads of Insight-HXMT, LE (1–10 keV), ME (10–30 keV), and HE (27–250 keV), respectively. For clarity, the phase is plotted from 0.7 to 1.7. The counts are normalized by scaling the counts of the main peak to unity and shifting the mean value of the background phase (0.6–0.8) to zero. The LE profile is significantly delayed by LE’s readout mechanism (see text for details).
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The top panel shows the periods of the Crab pulsar obtained by Insight-HXMT on different dates. The bottom panel shows the difference between our results and those from radio measurements at the Jodrell Bank observatory.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The top panel shows the best-fit values of the main pulse positions of the Crab pulsar using the timing ephemerides of NICER. The black points, red squares, and blue triangles are the results for HE, ME, and NICER respectively. The corresponding dotted lines are the mean phases for them. The bottom panel shows the best-fit values of the main pulse positions of Crab pulsar for LE. The purple dotted line is the mean phase for LE. The purple slashed area shows the 1σ (systematic error) confidence intervals for the mean phase.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: Radio delay of the main peak position for the Crab pulsar compared to the X-ray at different energies. The main peak delays of Insight-HXMT/HE and Insight-HXMT/ME with respect to NICER/XTI are calculated. Considering the radio delay of 304 μs compared to XTI reported in Enoto et al. (2021), we obtain the radio delay as a function of X-ray energy. The data are collected from NICER and Insight-HXMT, covering 1–250 keV. The black dashed line is the best fit to the data points of HE, ME, and XTI with a linear function. The purple NICER and black Insight-HXMT results are from this work. The radio delays of RXTE/PCA, HEXTE (red triangles), and INTEGRAL/SPI (blue triangles) reported in Molkov et al. (2010) are shifted downward by about 10 μs for comparison.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The upper diagram is the electronic design of the Insight-HXMT/HE, and the lower diagram indicates the internal instrumental delay of detected X-ray photons. The PPS signal and X-ray photons are recorded by the FPGA through different electronic processes. For the PPS signal, the GPS receiver (GPSR) receives the international atomic time (TAI) signal and then passes through a driver that produces a 10 ns delay. The PPS then travels at a speed of 5 nsm−1 over a cable of about 4 m to the HE electronic box. One receiver spends 19 ns in signal processing. The FPGA sampling process generates another 20 ns delay. For X-ray photons, after depositing in the NaI crystal, the photoelectrons are generated by the PMT and the transit time of PMT produces a delay of 115 ns. After three operational amplifiers (generating a delay of 15 ns) and through about 4 m of cable (about 20 ns delay), it reaches the HE electronic box. Through another operational amplifier (about 5 ns) and a comparator (generating a delay of 50 ns), it arrives at the FPGA and is recorded. A 20 ns of sampling time is also required for the FPGA to process the X-ray photons. The lower diagram indicates that the X-ray photons have an approximately 156 ns offset to the GPS PPS signal.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The upper diagram is the electronic design of the Insight-HXMT/ME, and the lower diagram indicates the internal instrumental delay of detected X-ray photons. For the PPS signal, the GPS receiver (GPSR) receives the international atomic time (TAI) signal and then passes through a driver that produces a 6 ns delay. The PPS then travels at a speed of 5 ns m−1 over a cable of about 4 m. Then it is processed by a receiver, which generates a 9 ns delay. In the ME electronic box, a signal passes through another driver (costs 2 ns), a 3 m cable (costs 15 ns), and another receiver (costs 3.4 ns) and is recorded by the FPGA. The FPGA sampling process generates a 312.5 ns delay. The total delay of PPS signal is about 367.9 ns, as indicated in the lower diagram. For X-ray photons, they are detected by Si-PIN detector. The charge sensitive amplifier processes the signal and produces a 10 ns delay. Through the ASIC (300 ns) and a comparator (80 ns delay), it recorded by the FPGA in the ME electronic box. The total delay of an X-ray photon is about 702.5 ns, as indicated in the lower diagram. The offset of X-ray photons compared to PPS is about 334.6 ns.
Paper: In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope
Authors: Youli Tuo, Xiaobo Li, Mingyu Ge, Jianyin Nie, Liming Song, Yupeng Xu, Shijie Zheng, Fangjun Lu, Shuang-Nan Zhang, Congzhan Liu, Xuelei Cao, Yong Chen, Jinlu Qu, Shu Zhang, Haisheng Zhao, Shuo Xiao, Baiyang Wu, Xiangyang Wen, Weichun Jiang, Bin Meng, Weiwei Cui, Wei Li, Yifei Zhang, Xufang Li, Yanji Yang, Ying Tan, and Bing Li
Figure caption: The upper diagram is the electronic design of the Insight-HXMT/LE, and the lower diagram indicates the internal instrumental delay of detected X-ray photons. For the PPS signal, the electronic processes are similar to the ME design. The GPS receiver (GPSR) receives the international atomic time (TAI) signal and then passes through a driver that produces a 10 ns delay. The PPS then travels at a speed of 5 ns m−1 over a cable of about 4 m. Then, it is processed by a receiver, which generates a 10 ns delay. In the LE electronic box, a signal passes through another driver, a 3 m cable, and another receiver and is recorded by the FPGA. The FPGA sampling process generates a 30 ns delay. The total delay of the PPS signal is about 105 ns, as indicated in the lower diagram. For X-ray photons detected by the LE SCD detectors, the delay is mainly contributed by the special readout mechanism. The main pulse of the Crab pulsar will be delayed by 856 μs. The total electronic processes produce about an 8 μs delay. Thus, the instrumental offset of X-ray photons of the LE is about 864 μs, as indicated in the lower diagram.
Paper: Linking Extragalactic Transients and Their Host Galaxy Properties: Transient Sample, Multiwavelength Host Identification, and Database Construction
Authors: Yu-Jing Qin, Ann Zabludoff, Marina Kisley, Yuantian Liu, Iair Arcavi, Kobus Barnard, Peter Behroozi, K. Decker French, Curtis McCully, and Nirav Merchant
Figure caption: Left: the cumulative distribution of transient redshifts in our database. The redshift axis is stretched so that events are uniformly distributed along the axis. Major supernova types, including Type Ia, Type II, and stripped-envelope (Ib, Ic), are highlighted here. Compared to Type II and SE SNe, SNe Ia generally have higher redshifts in our sample, likely due to their higher luminosities. Meanwhile, SE SNe are distributed at even lower redshifts than Type II. Other transients, mainly GRBs with redshifts reported, are distributed at the higher redshift side of our sample. Right: the fraction of each major type across the redshift range, with similar, stretched redshift so that the shaded area scales with number counts. Labels with ellipses count events of any subtype under this parent type, while labels with asterisks only include events without any subtype labels. A large fraction of events at low redshift are CC SNe, and the relative fraction of stripped-envelope SNe (SN Ib and Ic) within CC SNe drops with increasing the redshift. The contribution of SNe Ia increases with redshift and peaks near z ≃ 0.1, while subtypes of SNe Ia are mostly at the lower redshifts.