adsabs/AstroCLIMB huggingface dataset:
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: Top left: the display of the light curve for Sector 40 of HD 120084 is described with gray dots representing the original data and a green line showing the smoothed trend of variation. Right: display of the asteroseismic parameters obtained after analyzing the power spectrum with the pySYD package. Detailed descriptions of each figure can be found at this website: https://pysyd.readthedocs.io/en/latest/library/output.html. Bottom left: when the frequency separation is 6.41 μHz, the echelle diagram shows orange and red dots representing ν  n,0 and ν  n,2 as identified by PBjam. It is important to note that this frequency separation is not equivalent to the measured value of observed Δν.
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: Top left: the display of the light curve for Sector 40 of HD 29399 is described with gray dots representing the original data and a yellow line showing the smoothed trend of variation. Right: display of the asteroseismic parameters obtained after analyzing the power spectrum with the pySYD package. Detailed descriptions of each figure can be found at this website: https://pysyd.readthedocs.io/en/latest/library/output.html. Bottom left: when the frequency separation is 6.41 μHz, the echelle diagram shows orange and red dots representing ν  n,0 and ν  n,2 as identified by PBjam. It is important to note that this frequency separation is not equivalent to the measured value of observed Δν.
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: Left: the effective temperature–luminosity Hertzsprung–Russell diagram of HD 120084, with the gray line representing the evolutionary track of HD 120084 simulated numerically by MESA, and the red data points and error bars derived from the data in this work. Right: the effective temperature–surface gravity Hertzsprung–Russell diagram of HD 120084. The orange line (III) and green line (IV) represent the giants and subgiants, respectively; the red lines mark the positions of supergiants (II); and the blue lines mark the positions of dwarfs (V) (Straižys & Kuriliene 1981).
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: Left: the power spectrum of P(τ) for the host star HD 120084, ΔΠ1 for this star is 303.96 s. Right: the power spectrum of P(τ) for the host star HD 29399, ΔΠ1 for this star is 83.55 s.
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: Left: the effective temperature–luminosity Hertzsprung–Russell diagram of HD 29399, with the gray line representing the evolutionary track of HD 29399 simulated numerically by MESA, and the red data points and error bars derived from the data in this work. Right: the effective temperature–surface gravity Hertzsprung–Russell diagram of HD 29399.
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: HD 120084 corner diagram of asymptotic fit parameters.
Paper: Revealing the Fate of Exoplanet Systems: Asteroseismic Identification of Host Star in the Red Clump or Red Giant Branch
Authors: Wen-Xu Lin, Sheng-Bang Qian, Li-Ying Zhu
Figure caption: HD 29399 corner diagram of asymptotic fit parameters.
Paper: Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging
Authors: T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai, N. Raouafi
Figure caption: Long-duration (3.67 hr) PSP crossing of a sunward-directed HCS reconnection exhaust during E14. (a), (b) Proton and electron spectrograms in differential energy flux (eVs−1 cm−2 ster−1 eV−1); (c) pitch angle distribution of 640 eV electrons; (d), (e) magnetic field magnitude and components in RTN coordinates; (f) proton velocity in RTN; (g) density measured by SWEAP/SPAN-ion instrument (back) and from FIELDS/Quasi-Thermal Noise spectroscopy (red). The multi-island coalescence shown in panel (h) is from a kglobal simulation of reconnection (Yin et al. 2024) and serves as a sketch to illustrate the effective trajectory of PSP quickly crossing much of the HCS, followed by skimming near one edge of the HCS for a long time. The vertical blue dashed lines in panels (a)–(g) mark the edges of the HCS. The proton velocity is in the Sun’s frame, while the spectrograms are in the spacecraft frame. PSP remained inside the HCS during the entire 3.67 hr. Five SCSs exhibiting reconnection jets are labeled in panel (e).
Paper: Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging
Authors: T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai, N. Raouafi
Figure caption: Examples “2” and “3” of reconnection in SCSs embedded inside the HCS exhaust. Their locations are marked in Figure 1(e). (a), (e) Magnetic field in RTN; (b), (f) proton velocity in RTN; (c), (g) magnetic field in the XYZ SCS coordinate system; (d), (h) X component of the velocity. The parameters are the same as in Figure 2. The vertical blue dashed lines mark the two edges of the SCS based on magnetic field data, which have higher temporal resolution than proton data. The XYZ coordinate system is shown in Figure 4(i).
Paper: Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging
Authors: T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai, N. Raouafi
Figure caption: Example “1” of reconnection in the SCSs embedded inside the HCS exhaust. SCS “1b” is located at the trailing edge of SCS “1a.” Parameters a–h are the same as in Figure 2. (i) Schematic of the PSP crossing of possible secondary reconnection exhaust (shaded yellow) occurring at the trailing edge of the primary SCS reconnection exhaust.
Paper: Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging
Authors: T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai, N. Raouafi
Figure caption: Examples “4” and “5” of reconnection in the SCSs embedded inside the HCS exhaust. The parameters are the same as in Figure 2.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: 1D and 2D marginalized posteriors of mass, radius, and compactness inferred by ST-U for the different implementations of background constraints on the 3C50 data set. The shaded region in the 1D marginalized posterior denotes the 68.3% credible interval for the very last model listed in the legend. The contours in the 2D marginalized posterior for a given model denote the 68.3%, 95.4%, and 99.7% credible intervals, and the posterior for the last model in the legend is shaded. The dashed–dotted lines represent priors for these parameters (also for all other corner plots in this Letter). In the legend, 3C50 refers to the data set used; BKG refers to the background, and the two numbers that follow correspond to n  l  and n  u  (n  u  = X indicates an absence of an upper limit); and Δ-AGN refers to the inclusion of the Delta AGN spectra (scaled to 3C50 exposure time) when defining lower and upper background limits. The inferences differ vastly upon inclusion of an upper background limit.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Count-rate spectrum of the Delta data set, along with the space weather background estimate and a representative range of the attenuated AGN spectra. Green is the estimated AGN spectrum for NICER based on XMM-Newton observations from 2009, and the red band shows the range of fluxes observed in NICER pointings at the AGN.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Phase-folded PSR J0437−4715 (3C50) event data shown over two rotational cycles. We use 32 phase intervals (bins) per cycle, and the count numbers in bins separated by one cycle are identical for a given channel(s). The sum over all phase-channel pairs yields the total counts. The top panel displays the waveform obtained by summing the channels in the contiguous subset [30, 300). The bottom panel displays the phase-channel-resolved count numbers for the same channel subset, where the color bar represents counts per channel per two cycles.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Inferred background and spot contributions by ST-U in the absence of any background constraints (left) and in the presence of both lower and upper background constraints (right) involving the instrument background and the Delta AGN spectrum (scaled to 3C50 exposure time), as applied to the 3C50 data set. The inferred background constitutes the bulk of the observed data in the absence of an upper background constraint. For more details of the figure elements and notations, see caption of Figure 5 in Vinciguerra et al. (2024).
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Top panel: 3C50 data. Middle panel: posterior expected count numbers generated by the ST-U model when imposing both lower and upper background limits. Bottom panel: Poisson standardized residuals (c  ik  and d  ik  represent the model-generated and data counts resolved over phases i and channels k). Prominently visible systematic structures indicate poor model performance.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Projections of the inferred maximum-likelihood (ML) geometry by the high MULTINEST resolution CST+PDT run involving both lower and upper background constraints as viewed from the observer inclination (left) and from the north pole (right). Hot spots in the opposite hemispheres are indicated using dimmed colors. Lensing effects are not shown in these projections. The maximum-likelihood geometry consists of a ring encompassing the north pole and a two-temperature spot in the southern hemisphere.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Mass, radius, and compactness posteriors inferred by the high MULTINEST resolution CST+PDT runs, both in the absence of any background constraints and in the presence of lower and upper background constraints involving the instrument background and 3C50 AGN spectrum. The 2D marginalized posteriors of the latter model, which constitutes our headline result, are shaded in blue. Both runs infer highly consistent radius posteriors, with the background-constrained run consisting of a distribution tail that extends slightly more toward higher radii.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Mass, radius, and compactness posteriors inferred by the CST+PDT for the NICER-only run (default resolution) involving both lower and upper background limits and for the joint NICER–XMM run. The joint NICER–XMM run exhibits a bimodal structure not seen in any of the previous NICER-only analyses. The less compact mode agrees more with the background-constrained NICER-only analysis for this model.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Inferred background and spot contributions by the high MULTINEST CST+PDT runs in the absence of background constraints (left) and in the presence of both lower and upper 3C50 background limits (right) involving the instrument background and the 3C50 AGN spectrum, as applied to the 3C50 data set. Similar to the exploratory models, we once again infer a very high background contribution in the absence of upper limits.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Mass, radius, and compactness posteriors inferred by the ST+PDT model configuration for the different implementations of background constraints on the 3C50 data set. The inclusion of an upper background limit tightens the radius posterior and favors a more compact solution.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Radius, inclination, instrument scaling, and N H posteriors inferred by the high MULTINEST resolution CST+PDT runs for the two different implementations of background constraints on the 3C50 data set.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Radius and spot geometry posteriors inferred by the high MULTINEST resolution CST+PDT runs for the two different implementations of background constraints on the 3C50 data set.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Inferred background and spot contributions by ST+PDT in the absence of background constraints (left) and in the presence of both lower and upper 3C50 background limits (right) involving the instrument background and the 3C50 AGN spectrum, as applied to the 3C50 data set. Similarly to ST-U, this model also infers a very high background contribution in the absence of upper limits.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Top panel: 3C50 data. Middle panel: posterior expected count numbers generated by the high-resolution MULTINEST CST+PDT run when imposing both lower and upper background limits. Bottom panel: Poisson standardized residuals showing no apparent systematic structures, indicating that the model is capable of explaining the data well.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Inferred mass and radius posteriors for the different capable models explored in this Letter compared to mass–radius curves from EoS models. The shaded contours are the 68% and 95% credible regions for the high-res CST+PDT runs, and the remaining contours represent the 68% credible regions for the default-resolution CST+PDT and ST+PDT runs. The colored dashed–dotted lines are example mass–radius curves generated using one of the families of EoS models explored in Rutherford et al. (2024). It employs the Baym–Pethick–Sutherland crust EoS (Baym et al. 1971) at densities less than 0.5 times the nuclear saturation density n  s , the N3LO χEFT band from Keller et al. (2023) at densities of 0.5–1.5n  s , and a parameterized piecewise polytropic model (Hebeler et al. 2013) at higher densities. The parameters for the mass–radius relations shown here have been chosen to span the range of stiffness allowed by this model that is also compatible with the existence of ∼2.0 M ⊙ neutron stars.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: 1D and 2D marginalized posteriors inferred by ST-U when applied to the Delta (Δ) data set either using no background, using the space weather (SW) + elsewhere component, or informed by XMM-Newton (data and background).
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by ST-U as applied to the 3C50 data set, testing the different implementations of background constraints.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by ST+PDT as applied to the 3C50 data set, testing the different implementations of the 3C50 background constraints.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by ST+PDT as applied to the Delta data set with lower background constraints imposed by the space weather estimate.