Discovery of PSR J0125-5854, a 24 ms pulsar in a binary with orbital period ~834 days, low eccentricity, and likely helium white dwarf companion.
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and Tollerud, Erik J
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- method wards et al. 2006) v2024.12.1 to update the more accu- rate ephemeris of the source. Times of arrival (ToAs) were derived throughZ 2 searching, with the minimum phase in each profile serving as the ToA for the corre- sponding observation (Ge et al. 2012, 2019; Younes et al. 2020; Peng et al. 2026). For spectral analysis, we per- formed fitting using XSPEC (Arnaud 1996) v12.14.1, as part of HEASoft v6.34, which allowed us to model and analyze the spectra comprehensively. NICER data that partly ov
- method CXOU J191238.0+101043 is flatter than a single Gaussian function in radii larger than 5. ′′0. We then extracted the Chandra spectra from a 19. ′′0 radius circle centered on these sources. We performed a simple phenomenological fit with a power-law model in the 1-5 keV band, where the background is nearly negligible. We used XSPEC version 12.14.1 (K. A. Arnaud 1996) for the spectroscopy. The derived flux in the 2-10 keV band and power-law index are ∼1.5×10 −14 erg s −1 cm−2 and∼2.6 for CXOU J1912
- method 2025) indicate that the inclusion of DDO51 can substantially reduce the Teff-logg degeneracy inherent to broadband-only configurations. While the present work focuses on the data release and calibration of the DDO51 band, these results illustrate the expected role of DDO51 as the primary gravity-sensitive component of the SAGES system. The primary science drivers for the SAGES DDO51 observations include: (1) photometric pre-selection of giant stars for spectroscopic follow-up surveys; (2) large-
- method spectrum of 2CXO J0507 clearly shows hydrogen emis- sion lines and signatures of an M-dwarf donor (see Fig- ure 2), inconsistent with the helium-dominated donor, like in AM CVns (Ramsay et al. 2018) or helium CVs (Green et al. 2020). We performed additional Lomb- Scargle analysis using a two-term sinusoidal model to search for periodicity. We detected the strongest peak atP= 140.3211(2) min≈2.34 hr, which exceeds the 3σconfidence level. We identify this period as the or- bital period (orbital fr
- method the standardtardisradiation-field and plasma deter- 9 https://github.com/tardis-sn/tardis/tree/release-2025.03.23 Spectral Inference of SN 2014L5 T able 1.Model parameters and prior distributions tardisSample Grid a Inference Prior Parameter Distribution Range Parameter Distribution Range SN t[days] Uniform [8, 36] t[days] Uniform [8, 36] L[erg s −1] Log-uniform [6.31e+41, 3.98e+42] L[erg s −1] Log-uniform [6.31e+41, 3.98e+42] Densityb ρ0 [g cm−3 ] Log-uniform [3.16e-11, 1e-8] αρ c Uniform [-10,
- method To determine uncertainties, we bootstrap the datasets 10 5000 times for each model and epoch. In order to calculate flux as a function of wavelength, we employ an optically thin dust-emission model, Fν = κM d2 SN Bλ(λ, T).(3) We taked SN ≈36.0Mpc (Section 4.1), andB λ(λ, T)is the Planck blackbody function. The final parameter is the opac- ity, κ= 3 4ρa Qabs(λ),(4) whereQ abs is the absorption efficiency,ρis the density of the grain material, andais the average grain radius. We apply the optical
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JWST data show multiphase filaments feeding a circumnuclear disk that mediates accretion onto the black hole in NGC 4696, closing the AGN feedback loop.
Presents a fully photometric framework to measure individual cluster splashback radii and masses from SDSS data and constructs the first observational splashback mass function.
JWST nebular spectra detect cooling ~400 K carbonaceous dust emission in normal SN Ia 2023qov at +276 and +363 days, modeled as pre-existing circumstellar dust with mass ~10^{-4} M_sun located within ~1 light year.
Quantitative Bayesian inference using a deep-learning emulator detects 0.018-0.020 M_sun of helium in the Type Ic supernova 2014L.
First radio observations of SN 2023fyq detect a dense circumstellar shell with mass-loss rate ~0.004 solar masses per year ejected 0.7-3 years before explosion, consistent with a merger origin.
JWST timing observation detects pulsed IR emission from magnetar 4U 0142+61 matching its spin period, with flux 22.9±0.6 μJy and ~10% pulsed fraction lower limit.
First use of the learned harmonic mean estimator for Bayesian model selection across circular/eccentric, white-noise/GP, and trend variants in radial velocity exoplanet analyses.
Asteroseismic structure inversions can be performed in acoustic and buoyancy coordinates, overcoming breakdowns for non-solar stars and removing the need for prior mass and radius knowledge in p-mode cases.
JWST data revises Kamo`oalewa's spectrum to neutral colors consistent with enstatite-rich silicates, models its size at 18 m and albedo at 0.59, and confirms fast rotation.
First narrow-line flux ratios for lensed quasar RXJ1131-1231 measured with JWST/NIRSpec IFS at ~5% precision, detecting cusp anomaly consistent with prior work.
Time-resolved XRISM spectroscopy of NGC 4395 reveals variable inner-disk Fe Kα emission interpreted as Lense-Thirring precession, favoring low black hole mass (~9e3 solar masses) and moderate spin (a≳0.6).
Multi-epoch X-ray observations of SLSN-I 2018bsz support ejecta-CSM interaction as the dominant X-ray powering mechanism rather than a central magnetar.
Resolved multiphase observations reveal a supernova-driven wind in a z=5.3 galaxy removing gas at twice the star-formation rate, potentially quenching it within 100 Myr and matching local superwind properties.
Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.
JWST spectra of six z=5-9 galaxies show low-ionization covering fractions of 0.2-0.9 and diverse kinematics including blueshifted outflows, indicating heterogeneous multiphase ISM.
RUBIES JWST sample shows U increases with redshift and sSFR, decreases with mass, rising by a factor of ~4 from z=2 to z=6 at fixed mass and sSFR, with 0.3 dex systematic uncertainty from photoionization model range.
Blue straggler stars in old open clusters exhibit a Kraft break in rotation, with rapid rotators above the break and slow rotators below, indicating their envelopes behave like those of single stars.
The EDGES team publishes the first full public description of its 21-cm global-signal analysis pipeline, an open-source end-to-end software package, and the raw data from prior observations.
A 25-year Chandra catalog of 100 Sgr A* X-ray flares confirms that brighter flares are spectrally harder and strengthens prior correlations with duration and fluence.
A W-Net deep learning model detects asteroids in TESS data independently of trajectory by rotating training image cubes and using adaptive normalization for data scaling.
Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
ALMA Band 6 data detect SiO emission and masers up to v=8 in AGB stars, showing clumpy distributions, velocity gradients, and a tentative link between emission radius and mass-loss rate.
Detection of helium lines in Balmer-dominated shocks of Type Ia SNRs reveals enhanced helium in some remnants and challenges shock models, enabling new constraints on progenitor environments.
citing papers explorer
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JWST Nebular Spectroscopy of SN 2023qov: Circumstellar Dust Emission in a Normal Type Ia Supernova
JWST nebular spectra detect cooling ~400 K carbonaceous dust emission in normal SN Ia 2023qov at +276 and +363 days, modeled as pre-existing circumstellar dust with mass ~10^{-4} M_sun located within ~1 light year.
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Constraining the Galactic bar using the M92 stellar stream
Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
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The Tale of a Hungry Subgiant and Its Brown Dwarf: Interior Radiative Damping Dominates the Tidal Evolution of TOI-5882
A coupled MESA-GYRE framework shows interior radiative damping of gravity waves dominates tidal evolution in TOI-5882, predicting a 2-6 fold reduction in engulfment timescale versus equilibrium tide models.
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Isolating Sgr A East: The First Uncontaminated X-ray Maps of a Galactic Center Supernova Remnant
pGMCA separation of Chandra data yields the first uncontaminated X-ray maps of Sgr A East, with spectral fits showing lower ionization age and higher electron density than prior reports.
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The Critical Mass in Galaxy Evolution
A simulation study finds that a hot gas halo at galaxy total mass ~10^12.5 solar masses suppresses cool gas accretion, driving a redshift-independent turnover in the stellar-to-total mass ratio via reduced in-situ star formation efficiency.
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Uniform Reinterpretation of Rocky Exoplanet Secondary Eclipse Observations and the Impact of Stellar and Orbital Uncertainties
Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.
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Morphological complexity of NGC 628 - a multiwavelength multiscale analysis using the ordinal pattern framework
Multiwavelength analysis of NGC 628 using ordinal pattern measures finds a ~200 pc characteristic scale separating star-formation-driven structures from larger dynamical morphology, with C-H trajectories converging to an isotropic Gaussian random field attractor.
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Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova
No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
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Radial redistribution of stellar orbits in FIRE simulations of Milky-Way-mass galaxies
FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
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Investigating the Relationship Between Physical Properties and Spatial Irregularities at Coronal Hole Boundaries
Leading boundary of a coronal hole has higher plasma temperature, stronger unipolar field, and lower spatial irregularity than trailing boundary due to organized loops versus dispersed bipoles.
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Magnetic field alignment with dense cores in the transition between cloud and core scales
Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.
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Resolving the 2024 Outburst of Magnetar 1E 1841-045 from its host Supernova Remnant with EP-FXT
New EP-FXT data on the 2024 outburst of magnetar 1E 1841-045 shows energy-dependent multi-peaked pulses, spectral hardening, BB temperature-pulse intensity correlations, and effective separation from supernova remnant emission.
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LightCurveLynx: Forward Modeling of Time-Domain Surveys with Application to ZTF SN Ia DR2
LightCurveLynx is a flexible forward-modeling tool that produces supernova light-curve simulations matching ZTF observations with low KL divergence and consistent completeness limits.
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AGN STORM 2. XII. Ground-Based Optical Photometry and Lag Measurements of Mrk 817
Reverberation lags in Mrk 817 range 3-8 days, exceed thin-disk models by factors of 3-6, follow a λ^{4/3} trend with the ICCF method, and vary by up to a factor of 2 between epochs.