adsabs/AstroCLIMB huggingface dataset:
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Distribution of the best-fitting values for the break frequency in the relations between different spectral parameters and QPO frequency, as derived from the MCMC analysis.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: QPO fractional rms as a function of photon energy for ExpIDs with different QPO frequencies. Black, blue, and green points correspond to the ExpIDs P061433801101, P061433802405, and P061433802702, respectively.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Hardness ratio versus QPO frequency for the observations in the flaring state of Swift J1727.8–1613. The hardness ratio is defined as the ratio of the count rate in the ranges 4–10 and 2–4 keV. The red dotted line is the best-fitting curve using a power-law function.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Insight-HXMT LE 2–10 keV light curve and corresponding dynamical power spectrum with a time resolution of 64 s for the flaring period of Swift J1727.8–1613. All time gaps were removed, and the x-axis represents the index of the PDS.
Paper: The Prevalence of Bursty Star Formation in Low-mass Galaxies at z = 1–7 from Hα-to-UV Diagnostics
Authors: Marissa N. Perry, Anthony J. Taylor, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Vital Fernández, Pablo Arrabal Haro, Katherine Chworowsky, Nikko J. Cleri, Mark Dickinson, Richard S. Ellis, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Fabio Pacucci, Casey Papovich, Nor Pirzkal, Sandro Tacchella
Figure caption: Hα-based (left) and UV-continuum-based (right) SFRs vs. stellar masses for our galaxy sample binned by redshift. Vertical gray regions and gray data points indicate where our sample is not mass complete, as defined in Section 3.4. These data points are excluded from the fitting procedure. In the left panel, horizontal gray regions indicate the 5σ NIRSpec G395M grating emission-line sensitivity limits derived from Table 6 in S. L. Finkelstein et al. (2025). In the right panel, we compute 3σ limiting SFR(UV) values based on the faintest reliably measured rest-frame UV-continuum in each redshift bin, defined as the maximum of the 16th percentile M1500Å values from our SED-fitting posteriors of galaxies with S/N > 3. The colored shaded regions denote the 1σint intrinsic scatter intervals about the SFMS and its associated error. The black dashed and dashed–dotted curves represent literature values from P. Popesso et al. (2023) and J. S. Speagle et al. (2014), respectively. On average, the Hα-based SFMS and the UV-based SFMS exhibit the same degree of intrinsic scatter, indicating that we do not detect short-timescale (∼10 Myr) SFR variability across the sample with the SFMS.
Paper: The Prevalence of Bursty Star Formation in Low-mass Galaxies at z = 1–7 from Hα-to-UV Diagnostics
Authors: Marissa N. Perry, Anthony J. Taylor, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Vital Fernández, Pablo Arrabal Haro, Katherine Chworowsky, Nikko J. Cleri, Mark Dickinson, Richard S. Ellis, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Fabio Pacucci, Casey Papovich, Nor Pirzkal, Sandro Tacchella
Figure caption: The fraction of galaxies whose Hα-to-UV ratios are consistent (middle panel) and inconsistent (outer panels) with a constant SFH computed by V. Mehta et al. (2023) shown as a function of redshift. For each stellar mass and redshift bin, we perturb the observed ratios using Gaussian noise based on 1σ errors and compute fractions via bootstrap resampling. Measured values correspond to the median of the bootstrap distribution, with error bars from the 16th and 84th percentiles. Colored curves represent this work, binned by stellar mass and redshift, compared to the dotted gray curve from L. Clarke et al. (2024), which includes galaxies with stellar masses in the range 107–1010.5M*/M⊙. Within each bin, we compute the median redshift value. We estimate uncertainties on the fractions using bootstrap resampling. These trends suggest little evolution in the relative fraction of galaxies above, below, or within the equilibrium range over z = 1–7.
Paper: The Prevalence of Bursty Star Formation in Low-mass Galaxies at z = 1–7 from Hα-to-UV Diagnostics
Authors: Marissa N. Perry, Anthony J. Taylor, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Vital Fernández, Pablo Arrabal Haro, Katherine Chworowsky, Nikko J. Cleri, Mark Dickinson, Richard S. Ellis, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Fabio Pacucci, Casey Papovich, Nor Pirzkal, Sandro Tacchella
Figure caption: Left panel: the Hα-to-UV ratio vs. stellar mass for our galaxy sample binned by stellar mass. The large points represent the median values in each stellar mass bin. The vertical error bars denote the 16th and 84th percentiles of each bin and the horizontal error bars denote the stellar mass range of each bin. The horizontal gray hatched region shows the equilibrium range of the Hα-to-UV ratio calculated by V. Mehta et al. (2023). Right panel: the Hα-to-UV ratio vs. redshift for our galaxy sample binned by stellar mass. The large points represent the median values in each stellar mass and redshift bin. The vertical error bars denote the 16th and 84th percentiles of each bin and the horizontal error bars denote the redshift range of each bin. Lower-mass galaxies maintain higher Hα-to-UV ratio values across all redshifts probed compared to higher-mass galaxies, suggesting lower-mass galaxies are more prone to bursty star formation.
Paper: The Prevalence of Bursty Star Formation in Low-mass Galaxies at z = 1–7 from Hα-to-UV Diagnostics
Authors: Marissa N. Perry, Anthony J. Taylor, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Vital Fernández, Pablo Arrabal Haro, Katherine Chworowsky, Nikko J. Cleri, Mark Dickinson, Richard S. Ellis, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Fabio Pacucci, Casey Papovich, Nor Pirzkal, Sandro Tacchella
Figure caption: The distribution of Hα-to-UV ratio values binned by redshift. The vertical gray hatched region shows the equilibrium range of the Hα-to-UV ratio calculated by V. Mehta et al. (2023). For each redshift bin, the distribution peak lies within the equilibrium range expected for a constant SFH over the past ∼100 Myr.
Paper: The Prevalence of Bursty Star Formation in Low-mass Galaxies at z = 1–7 from Hα-to-UV Diagnostics
Authors: Marissa N. Perry, Anthony J. Taylor, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Vital Fernández, Pablo Arrabal Haro, Katherine Chworowsky, Nikko J. Cleri, Mark Dickinson, Richard S. Ellis, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Fabio Pacucci, Casey Papovich, Nor Pirzkal, Sandro Tacchella
Figure caption: Spectroscopic redshift distribution of our sample split by survey (top) and by redshift bin (bottom). The full sample consists of 346 spectroscopically confirmed galaxies. We divide the sample into four redshift bins: z = 1–2.5, z = 2.5–4, z = 4–5.5, and z = 5.5–7, which we use throughout our analysis to examine redshift evolution in galaxy properties across cosmic time.
Paper: Constraints on Diffuse X-Ray Emission from the TeV Halo Candidate HESS J1813-126
Authors: David Guevel, Kim L. Page, Kaya Mori, Amy Lien, Ke Fang
Figure caption: The region surrounding HESS J1813-126 is shown above. The color indicates the significance of the HAWC detection, with the thick dashed black line indicating the 3σ level. The HAWC significance maps are produced with public data. (The HAWC public data were retrieved from https://data.hawc-observatory.org/datasets/3hwc-survey/index.php) The likelihood is calculated as if there is a point source present at the center of each pixel in a HEALPIX pixelation of the sky. The normalization of the source is varied until the likelihood is maximized, assuming a spectral index of 2.5. The statistical significance is evaluated as the square root of the log-likelihood ratio (A. Albert et al. 2020). The thin black circles show the Swift-XRT field of view centered on the observed targets. 4U 1812-12, PSR J1813-1246, and V* NP Ser are shown as a plus, cross, and star.
Paper: Constraints on Diffuse X-Ray Emission from the TeV Halo Candidate HESS J1813-126
Authors: David Guevel, Kim L. Page, Kaya Mori, Amy Lien, Ke Fang
Figure caption: The spectral energy distribution for the TeV halo HESS J1813-126 with Swift-XRT upper limits (left) and the spectral energy distribution of the pulsar itself (right). The TeV emission is produced by IC scattering, primarily with the cosmic microwave background, though there is a small contribution from the stellar ISRF (ISRF-star) and the infrared ISRF (ISRF-IR). The synchrotron radiation is produced by the same population of energetic electrons with a magnetic field of uniform strength.
Paper: Constraints on Diffuse X-Ray Emission from the TeV Halo Candidate HESS J1813-126
Authors: David Guevel, Kim L. Page, Kaya Mori, Amy Lien, Ke Fang
Figure caption: The 2–5 keV flux maps for targets 1, 2, and 3 are shown with the composite flux map from the archival observation. The maps are binned in 10 by 10 superpixels, then divided by the binned exposure map. The detected point sources are shown in red circles. PSR J1813-1246 is also circled in orange, and the HESS best-fit location, location uncertainty, and best-fit extension are shown in teal. The HAWC 5σ significance is shown by the gray dashed line.
Paper: Constraints on Diffuse X-Ray Emission from the TeV Halo Candidate HESS J1813-126
Authors: David Guevel, Kim L. Page, Kaya Mori, Amy Lien, Ke Fang
Figure caption: The X-ray surface brightness for the four fields is shown as a function of distance from PSR J1813-1246 after excluding point sources and bright Earth contamination. The vertical error bars are the statistical Poisson uncertainty. The horizontal error bars are not statistical; they represent the angular extent of the Swift-XRT field of view. The innermost observation slightly overlaps with the pulsar location, so the errors appear beyond zero radius.
Paper: Constraints on Diffuse X-Ray Emission from the TeV Halo Candidate HESS J1813-126
Authors: David Guevel, Kim L. Page, Kaya Mori, Amy Lien, Ke Fang
Figure caption: Spectra for the archival observations (black), Field 1 (red), Field 2 (green), and Field 3 (blue). The spectra have been produced after removing bright Earth contamination and point sources. The fluxes of the spectra are grossly compatible and consistent with GRXB and CXB.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: Dynamics of the erupting filament EF in AIA 304 Å and the IRIS SJI bidirectional reconnection outflows. (a) The AIA 304 Å time–distance map shows the height variations of filament EF and the overlying compressed prominence material in Barb1 during the eruption. The yellow dashed horizontal line indicates the solar surface. Panels (b) and (c) display the velocity-time and acceleration-time profiles of EF (red) and the overlying prominence material (blue) with 1σ (standard deviation) error bars. (d) IRIS 1400 Å time–distance slit image enhanced by the MGN method presents six pairs of bidirectional reconnection outflows (o1–o6). The circles mark the spots where the reconnection outflows originated. (e) The projected velocity distribution of the reconnection outflows with 1σ error bars. The purple and green dotted lines represent the mean projected velocities of the reconnection outflows moving toward C and D, respectively.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: IRIS spectral observations of the reconnection outflow. (a–c) Temporal evolutions of peak intensity, Doppler shift and line width derived from a single-Gaussian fitting to the spectra of Si IV 1393.76 Å line at T = 0.08 MK. The two vertical lines in panels (a), (b), and (c) indicate the time when the two reconnection outflows in panels (d) and (g) were observed by IRIS. Panels (d)–(f) and (g)–(i) show the IRIS 1400 Å imaging data, Si IV 1394 Å line spectrum, and profile of the reconnection outflow at 07:51:29 UT and 08:08:34 UT, respectively. The cyan arrows in panels (d) and (g) indicate the motion direction of the two reconnection outflows. The plus signs in panels (d) and (g) mark the sites where the reconnection outflows crossed the spectrometer slit. The blue (red) dotted curve in panels (f) and (i) is the single-Gaussian fitting profile with 1σ uncertainty.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: Magnetofrictional simulation of a quiescent prominence magnetic field driven by supergranulations. (a) Magnetic field lines of a bipolar potential magnetic field at time 0 as the initial condition in the spherical coordinates of a partial southern hemisphere. (b) Sheared magnetic arcades in rainbow colors and overlying potential magnetic loops in white at time 11.4. (c) Thin magnetic flux rope consisting of helical magnetic field lines in rainbow colors and overlying potential magnetic loops in white at time 18. (d) Side view of the simulated prominence at the solar limb presented by translucent magnetic dip regions colored by solar radii in red-to-blue colors and a green helical magnetic field line passing through the middle region of a prominence foot. (e) Top view of the same data as in (d) as a filament on the solar disk with additional white helical field lines presenting the structure of a magnetic flux rope at time 108. The bottom surfaces of all panels in black and white presenting photospheric magnetograms Br.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: The field orientation of the magnetic dip indicated by reconnection outflows across Barb1. (a) The cyan dashed profile of the bidirectional reconnection outflows at 07:56:17 UT (see Figure 6 (g)) overlaid on the KSO Hα intensity data. X- and Z-axes represent the local horizontal and upward directions, respectively. The black curve denotes the solar limb. (b) The variations of the angle (φ, diamond and dotted curve) between the dip field and x-axis and the curvature radius (square) projected in the plane of the sky of the dip bottom with 1σ error bars. The plus signs in panel (a) and vertical lines in panel (b) indicate the boundaries of Barb1.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: (a) The positions of STEREO A and B at 07:46 UT on 2014 April 8, obtained from the online STEREO orbit tool of the website (https://stereo-ssc.nascom.nasa.gov/where.shtml). The SDO AIA (b) and STEREO B EUVI (c) 304 Å intensity images show Barb1 and EF at the same time. The dashed lines in panels (b) and (c) are the longitudinal lines of −90°. The green (P1–P4) and white (P5–P6) plus signs denote the points at Barb1 and EF selected for the longitude calculations.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: The GONG Hα (a)–(b) and SDO AIA 304 Å (c)–(d) intensity images at 02:20 UT on April 13. The rectangles in panels (a) and (c) correspond to the FOVs of panels (b) and (d). The plus signs approximately indicate the footpoint of Barb1.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: Analysis of the GRB 250702E lightcurve. Top panel: the 256 ms binned lightcurve of GRB 250702E (n8) in the energy band of 8–1000 keV. Middle panel: the PSD of FFT. The dashed–dotted line shows the best-fit noise model, with green (95%), yellow (99%), and red (3σ) dashed lines showing the confidence intervals. Bottom-left panel: WWZ power. Bottom-right panel: WWZ time-integrated PSD and FFT PSD. Besides the QPO signal at 0.024 Hz, another possible QPO signal at 0.096 Hz that is exceeding 3σ confidence level is noted here. However, this QPO signal is only detected in n8 detector, while it is not shown in the lightcurves from other detectors. Thus, we are not sure of this identification as a possible QPO signal.
Paper: Magnetic Dip Found in a Quiescent Prominence Foot via Observation and Simulation
Authors: Huadong Chen, 华东 陈, Chun Xia, 莼 夏, Suli Ma, 素丽 马, Yingna Su, 英娜 宿, Guiping Zhou, 桂萍 周, Eric Priest, Lyndsay Fletcher, Yuandeng Shen, 远灯 申, Weining Tu, 炜宁 屠, Wei Wang, 威 王, Jun Zhang, 军 张
Figure caption: Schematic diagram of magnetic field structure of the larger-scale filament and its reconnection with the fields of the filament EF under Barb1. (a)–(b) Top and side view of the filament field structure, respectively. (c)–(e) The filament EF’s eruption and its interactions with the magnetic dip in Barb1. The box in panel (b) marks the FOV of panels (c)–(e). The dark gray cylinders represent the vertical threads in the barbs.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: Analysis of the GRB 250702D lightcurve. Top panel: the 256 ms binned lightcurve of GRB 250702D (nb) in the energy band of 8–1000 keV. Middle panel: the PSD of FFT. The dashed–dotted line shows the best-fit noise model, with green (95%), yellow (99%), and red (3σ) dashed lines showing the confidence intervals. Bottom-left panel: WWZ power. Bottom-right panel: WWZ time-integrated PSD and FFT PSD.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: Top panels: PSDs obtained from AR(2) spectral analysis of GRB 250702B lightcurves with 256 (left) and 16 ms (right) time bins. Bottom panels: PSDs obtained from AR(2) spectral analysis of GRB 250702E lightcurves with 256 (left) and 16 ms (right) time bins.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: Top panel: PSD comparison between FFT (blue solid line) and AR(2) model (purple dashed–dotted line) for GRB 250702B. Dashed lines show AR(2) confidence levels: green (95%), yellow (99%), and red (3σ). Bottom panel: same as top panel but for GRB 250702E. To clearly show the possible QPO signals compared to the AR(2) model, the low-frequency (<10−2 Hz) region is not displayed in this figure.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: The spectrum of GRB 250702DBE fitted with the Band function. The black data points are from the NaI (nb) detector, while the red data points are from the BGO (b1) detector. The solid stepped line shows the Band function fitting.
Paper: Possible Quasiperiodic Oscillation Signals in the Unique Event of GRB 250702DBE/EP250702a?
Authors: Fei-Fan Song, Jirong Mao
Figure caption: Analysis of the GRB 250702B lightcurve. Top panel: the 256 ms binned lightcurve of GRB 250702B (nb) in the energy band of 8–1000 keV. Middle panel: the PSD of FFT. The dashed–dotted line shows the best-fit noise model, with green (95%), yellow (99%), and red (3σ) dashed lines showing the confidence intervals. Bottom-left panel: WWZ power. Bottom-right panel: WWZ time-integrated PSD and FFT PSD.
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Histogram showing the discovery year of spider systems included in SpiderCat, color coded by spider subclass. The discovery year is defined as the year in which a paper was published confirming the system as a spider or spider candidate, or reporting the detection of millisecond pulsations from the source. The first four spider systems are highlighted. The dramatic increase in discoveries following the launch of the Fermi γ-ray Space Telescope reflects its critical role in guiding targeted radio (e.g., 350 MHz Green Bank Telescope (GBT) and 327 MHz Arecibo surveys) and multiwavelength surveys.
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Histogram of estimated Galactic heights for spider systems (bin size: 0.33 kpc), color coded by spider subclass. The distribution is approximately normal, with a mean height of ﹩\bar{z}=0.14\,\pm \,0.09﹩ kpc and a standard deviation of σz = 0.93 ± 0.06 kpc, overplotted as a scaled Gaussian (dashed line).
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Galactic distribution of spider systems in a Mollweide projection, color coded by spider subclass. The top and left panels show histograms of Galactic longitude (bin size: 12﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4) and latitude (bin size: 9﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5), respectively. The spider population is strongly concentrated toward low Galactic latitudes, while the distribution in Galactic longitude is relatively uniform.