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Physics Astrophysics

astro-ph Watch Astrophysics

Friday 3 April

Astrophysics of Galaxies

A Five-Stage Framework for Slitless Grism Spectra: Demonstrated on Euclid Q1 Strong-Lens Candidates and Ported to CEERS NIRCam

R.Tata

Wide-field slitless grism spectroscopy is difficult in the co-spatial regime, where multiple sources share one cross-dispersion PSF element and catalogue-level decontamination (aXe/LINEAR/Grizli) does not apply – the regime of strong lenses, binary AGN, and mergers in HST, JWST, Euclid, and Roman grism data. This paper presents a five-stage framework for per-source 1-D spectra and redshifts: distortion-calibrated extraction, Fourier/Sersic/NNLS deblending, robust-PCA cleaning, weighted friend-of-friend with Hungarian cross-orientation matching, and a Bayesian posterior layer. Of 579 published Euclid Q1 lens candidates, 473 fall in the NISP footprint. A 3" DESI DR1 Iron match gives 57 counterparts (51 ZWARN=0, 46 clean v6d anchors). Extending to 9200 A adds features below 12500 A in 312 source and 324 deflector spectra. Source/deflector features are detected in 467/471 of 473; 371 source redshifts are secure, 75 probable, 21 tentative. Adopted z_def is filled for 440/473 (55 DESI + 385 PHZ MODE_1). Catalogue: 342 complete, 29 source-only, 75 Silver, 21 Bronze, 6 none. Posteriors succeed for 398/473; DESI deflector coverage is 0.67+/-0.07 (46 anchors). Tiers platinum/gold/silver/bronze/none = 62/230/82/24/75. Median source 68% CI is dz=1.30; DESI |dz|<0.1 recovery is 35%. Source-side support is synthetic-only; the full deblender's real-data performance is unmeasured here. A ported v6c on 10 CEERS DR0.7 JWST/NIRCam targets improves median |dz|/(1+z) from 0.43 to 0.18, recovers 4/10 within 0.10, and contains truth in the 68% CI for 8/10 – portability across instruments, not independent calibration. The release is a 473-row catalogue with deflector redshifts, posterior intervals, and quality tiers.
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High Energy Astrophysical Phenomena

What Are Pulsar Companions Made of? Using Gravitational Tides to Probe Their Compositions

Liam Colombo-Murphy, Lucas Brown, Stefano Profumo et al. (+2 more)

Low eccentricity, short orbital period pulsar companions may provide a probe to study novel dense and stable exoplanet internal compositions due to the potentially significant orbital evolution they experience caused by strong gravitational tides. We model the tidal characteristics such as apsidal motion constants, orbital precession, and tidal deformability for a variety of equations of state to be compared with values recovered via pulsar timing for a sample of four systems: PSR J1719-1438b, PSR J0636+5128b, PSR J2322+2650b, and PSR J1807-2459A b. With this method, we hope to place stringent limits on the chemical and structural composition of these objects. Through limiting the internal composition of pulsar companions, we aim to elucidate their unique history and formation.
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All authors Liam Colombo-Murphy, Lucas Brown, Stefano Profumo, M. Grant Roberts, Aya Westerling

Astrophysics of Galaxies

The Stellar "Snake"-III: Co-evolution of Stars and Molecular Clouds Unveiled by Gaia, MWISP, and LAMOST

Jia-Peng Li, Hai-Jun Tian, Chen Wang et al. (+2 more)

By combining multi-band data from Gaia DR3, MWISP CO, and LAMOST DR11 LSR/MSR, we investigate the co-evolution of stars and their parent molecular cloud in a snake-like stellar structure, named Snake III. Based on 5-D phase-space selection, we identified 5683 member stars (median age 7.6 Myr) across approximately $300 \times 500 \times 175$ pc$^3$ volume, along with 12 embedded open clusters. Then we use BEEP distances combined with $^{12}$CO velocities to clearly identify the molecular clouds associated with the stellar complex in spatial and kinematics. The molecular cloud density increases with Galactic longitude, with older open clusters forming in cavities near higher-density regions (except ASCC 125), while young field stars currently form preferentially in present-day high-density environments, indicating that cloud density regulates the star-formation sequence. $^{12}$CO excitation temperature, centroid velocity, velocity dispersion and H$\alpha$ emission reveal that early feedback first compresses cloud edges to trigger new stars, then sweeps and disperses the parent clouds. The extremely young cluster (ASCC 125, 4.4 Myr) lies near the densest region yet is surrounded by a shell with bidirectional density-velocity perturbations, consistent with a delayed-triggering scenario under the combined influence of UBC 178 stellar-wind feedback and a suspected supernova blast. Our results naturally demonstrate that snake-like stellar structures are filamentary relics of hierarchical star formation within giant molecular clouds. They provide direct observational evidence that cloud density and early feedback jointly modulate the progression of star formation, offering a clear and young laboratory for studying star-cloud co-evolution.
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All authors Jia-Peng Li, Hai-Jun Tian, Chen Wang, Xiang-Ming Yang, Fan Wang

Solar and Stellar Astrophysics

The accretion-driven eruption of the recurrent nova T Corona Borealis

Raymundo Baptista, Wagner Schlindwein and Gerardo J. M. Luna

T Corona Borealis (T CrB) is a symbiotic recurrent nova with an $\simeq 80$ yr recurrence interval, the eruptions of which occur on top of a $\simeq 15$ yr long high-brightness state. We show that the high-brightness state is best explained as the response of a high-viscosity ($\alpha=3$) accretion disk to a unique event in which the mass transfer rate from the donor star increases by a factor $\simeq 100$, from $\dot{M}\mathrm{(quies)}= 2 \times 10^{-9} M_\odot$ yr$^{-1}$ up to $\dot{M}\mathrm{(out)}= 1.9 \times 10^{-7} M_\odot$ yr$^{-1}$; it can not be a thermal-viscous disk instability outburst neither a steady nuclear burning event. The constraint that the matter accreted onto the white dwarf in between eruptions equals the envelope mass $M_{ig}$ needed to trigger nova eruptions at the observed recurrence interval requires a white dwarf mass of $M_1= 1.29 M_\odot$, a donor star mass of $M_2= 0.7 M_\odot$, and an inclination of $i= 57.3^o$. As the high-brightness state responds for 95% of $M_{ig}$, the nova eruptions of T CrB are induced by accretion events. Without the 15 yr long enhanced mass transfer events, its nova recurrence interval would be significantly longer, $\simeq 5500$ yr. T CrB exhibits a conspicuous decrease in brightness during the 1-2 yr prior to the nova event. We argue that this pre-eruption dip occurs during the convection phase that precedes the nova eruption and is best explained by the slow, accelerated expansion of the accreted envelope (and inner disk radius) at an average velocity of $v_\mathrm{exp}= 0.02$ km s$^{-1}$ over a 2 yr timescale, likely as a consequence of excess heat being increasingly deposited at the accreted layer by thermonuclear reactions before the nova eruption stage.
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Solar and Stellar Astrophysics

The dwarf nova EX Draconis: a short review

Raymundo Baptista and Wagner Schlindwein

EX Draconis (EX Dra) is a long period dwarf nova showing ~2 mag outburst which lasts for ~7 d and recur on a timescale of (20-30) d. Its deep eclipses allows one to trace the changes in surface brightness and radius of its accretion disk along the outburst cycle and to perform critical tests of the predictions of the thermal-viscous disk instability (DI) and the mass transfer outburst (MTO) models proposed to explain dwarf nova outbursts. The results of four critical tests are in clear contradiction with DI while in good agreement with MTO expectations. Furthermore, the observed variations in brightness and outer disk radius throughout EX Dra outbursts are well described by the response of a high-viscosity (alpha = 3-4) accretion disk to events in which the mass transfer rate increases by factors of ~30 for ~7 d, in line with MTO expectations. We further argue that the old expectation of accretion disk theory, alpha <= 1, seems unjustified and contradicts the values derived from dwarf nova outburst decline timescales if they are driven by MTO.
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High Energy Astrophysical Phenomena

Pulsar scintillation studies with LOFAR III. Annual variations in PSR~J0814$+$7429

Yanqing Cai, Ziwei Wu, Weiwei Zhu et al. (+27 more)

The interstellar scintillation observed in radio pulsars arises from interference between electromagnetic waves scattered by electron density fluctuations in the turbulent interstellar plasma, providing a critical tool for probing the small-scale structure of the ionized interstellar medium and the pulsar system itself. The primary aim of this work is to study long-term scintillation variations for a bright and nearby pulsar, PSR J0814$+$7429, carried out from 2013 September to 2023 September with the LOw-Frequency ARray (LOFAR) High Band Antennae in the frequency range of 120 - 170 MHz. We derive the basic scintillation parameters, scintillation bandwidth ($\Delta\nu_{\rm d}$) and scintillation timescale ($\Delta\tau_{\rm d}$), from the two-dimensional (2D) auto-covariance function of the dynamic spectra that are a 2D matrix of pulse intensity as a function of time and frequency. We present the long-term monitoring of $\Delta\nu_{\rm d}$ and $\Delta\tau_{\rm d}$ for PSR J0814$+7429$, which shows a strong annual variation in the time series of the $\Delta\tau_{\rm d}$. From our modeling of the annual variations of scintillation velocities, the scattering screen is anisotropic and located at $0.23\pm0.02$ kpc from the Earth, likely corresponding to the boundary of the Local Bubble.
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All authors Yanqing Cai, Ziwei Wu, Weiwei Zhu, Joris P. W. Verbiest, Yulan Liu, Krishnakumar Moochickal Ambalappat, Marcus Brüggen, Benedetta Ciardi, Ralf-Jürgen Dettmar, Ziyao Fang, Qiuyang Fu, Matthias Hoeft, Jiawei Jin, Lars Künkel, Jörn Künsemöller, Caisong Liu, Lingqi Meng, Xueli Miao, Jiarui Niu, Rukiya Rejep, Dominik J. Schwarz, Golam M. Shaifullah, Caterina Tiburzi, Christian Vocks, Olaf Wucknitz, Mengyao Xue, Mao Yuan, Youling Yue, Chunfeng Zhang, Zhen Zhang

Instrumentation and Methods for Astrophysics · Cross-listed from stat.ME

A comparison of methods for Poisson regression in the presence of background

Massimiliano Bonamente, Vinay Kashyap, Xiaoli Li et al. (+1 more)

This paper provides a statistical analysis of three common methods of regression for Poisson data in the presence of Poisson background, namely the joint fit with two parametric models for the source and the background, the use of a non-parametric model for the background known as the wstat method, and the regression with a fixed background. The non-parametric background method, which is a popular method for spectral data, is found to be significantly biased, especially in the low-count and background-dominated regimes. Similar conclusions apply to the fixed-background regression. The joint-fit method, on the other hand, simultaneously affords reliable hypothesis testing by means of the usual Cash statistic and unbiased reconstruction of source parameters. We also investigate the effect of non-parametric regression on the number of effective degrees of freedom by means of the Efron degree of freedom function. We find that the wstat method adds a significantly larger number of degrees of freedom, compared to the number of free parameters in the source model. The other two methods have a number of degrees of freedom consistent with the number of adjustable parameters, at least for the simple models investigated in this paper.
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All authors Massimiliano Bonamente, Vinay Kashyap, Xiaoli Li, Jelle de Plaa

Earth and Planetary Astrophysics

Monitoring Volatile Evolution in Disrupting Comet D/2021 A1 (Leonard) with NOEMA and APEX

Timothy N. Proudkii, Nathan X. Roth, Jérémie Boissier et al. (+8 more)

We report a pre-perihelion survey of volatile emissions from comet D/2021 A1 (Leonard) with the Northern Extended Millimeter Array (NOEMA; UT 2021 Nov. 5, 21, and Dec. 1) and the Atacama Pathfinder Experiment (APEX; UT 2021 Dec. 9-10), spanning heliocentric distances ($r_H$) from 1.3 to 0.80 au. We securely detected HCN and CS and place 3$\sigma$ upper limits on CH$_3$OH, H$_2$CO, and CO abundances. Line kinematics and NOEMA spatial constraints indicate that HCN was released at or near the nucleus (parent scale length $<300$ km), while CS showed higher gas expansion velocities and mixing ratios that increased with decreasing $r_H$ $-$ consistent with production from a distributed source. Across our campaign, CS mixing ratios relative to H$_2$O increased by a factor of $\sim$5, from $0.02 \pm 0.01\%$ at $r_H$ = 1.3 au to $0.10\pm0.02\%$ by $r_H$ = 0.80 au. HCN mixing ratios in our data rose modestly, from $0.04 \pm 0.02\%$ at $r_H$ = 1.3 au to $0.07 \pm 0.02\%$ by $r_H$ = 0.81 au. However, contemporaneous measurements from other facilities placed HCN consistently at a higher absolute level ($\sim\!0.08\%$) with additional variability. Once cross-facility measurements were included, the HCN abundance showed no statistically robust monotonic dependence on $r_H$. Variability in both species during the mid-December outbursts and fragmentation suggests that D/2021 A1's volatile evolution reflected not only solar insolation but also disruption processes, underscoring the value of multi-epoch, multi-instrument monitoring to capture rapid, species-dependent changes.
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All authors Timothy N. Proudkii, Nathan X. Roth, Jérémie Boissier, Dominique Bockelée-Morvan, Nicolas Biver, Steven B. Charnley, Stefanie N. Milam, Martin A. Cordiner, Michael A. DiSanti, Boncho P. Bonev, Neil Dello Russo

Thursday 2 April

Astrophysics of Galaxies

Enhancement of the Rate of Tidal Disruption Events in Active Galactic Nuclei due to the Sweeping Secular Resonance Mechanism

Xiaochen Zheng, Morgan MacLeod, Douglas N. C. Lin et al. (+2 more)

Tidal disruption event (TDE) rates in active galactic nuclei (AGN) consistently exceed predictions from two-body relaxation, particularly in post-starburst and green valley galaxies. We explain this excess with a new mechanism: a sweeping secular resonance (SSR) driven by an intermediate-mass companion (IMC) and a depleting gaseous disk. As the disk mass declines, a resonance between stellar and IMC orbital precession sweeps through the nuclear cluster, exciting stellar eccentricities to near unity on orbital timescales far faster than gravitational relaxation. Our analytical framework, validated by N-body simulations (REBOUND), shows this mechanism requires IMC-to-SMBH mass ratios of $q \geq 10^{-3}$, disk mass ratio $p \geq 10^{-3}$, and few Myr-scale disk depletion. It is highly effective for co-orbiting IMCs but negligible for counter-orbiting ones. The TDE rate peaks at $10^{-3}-10^{-2}$ per galaxy per year for a depletion timescale $\tau_{\rm dep} \sim 10$ Myr. Even lower-mass IMCs can produce significant enhancements with compact, long-lived disks. Our model naturally explains elevated AGN TDE rates and implies that a high TDE incidence is a potential tracer of hidden parsec-scale IMCs, offering testable predictions for future AGN monitoring.
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All authors Xiaochen Zheng, Morgan MacLeod, Douglas N. C. Lin, Yi Yang, Zhenzhen Shao

Astrophysics of Galaxies

Spectroscopic confirmation of dual and offset quasars from the Subaru HSC-SSP program

Shenli Tang, John Silverman, Xavier Prochaska et al. (+4 more)

We present a spectroscopic follow-up program targeting closely-separated dual quasar candidates selected from imaging of SDSS quasars with the Subaru Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using two-dimensional image decomposition, our selection identifies PSF-like companions within 0.6-4 arcsec separation (< 30 kpc) around the SDSS quasar. We newly confirm six broad-line dual quasars and eleven offset quasars (quasar-galaxy pairs), spanning 1.5 < z < 3.3 for the duals and predominantly z < 0.6 for the offset systems. No obvious lensed quasars were discovered from this program. We obtained 99 spectra of these candidates from NTT/EFOSC2, Gemini/GMOS-N, Keck/NIRES, and Subaru/FOCAS. From the spectra, we measure the emission-line properties of these dual black holes (BH). At z > 1.5, the confirmed duals exhibit high black hole mass ($M_{\rm BH}$ $=10^{8.5}$-$10^{10} M_{\odot}$) with high bolometric luminosities ($L_{bol}$ $=10^{45.5}$-$10^{47.5}$ erg s$^{-1}$), yet accrete at moderate Eddington ratios ($\lambda_{\rm Edd}=$0.01-0.4). From the spectroscopically-confirmed samples, we estimate the dual fraction of SDSS quasars with separations of 0.6-4 arcsec to be 0.2%-1.2% at z<0.8, 0.08%-0.24% at 0.8<z<1.5, and 0.06% at 1.5<z<3.3. These values are broadly consistent with other recent optical studies, but lower than theoretical expectations of a rising dual fraction at cosmic noon. However, we note that these fractions, especially at high $z$, still need a more accurate assessment of selection and observation effects.
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All authors Shenli Tang, John Silverman, Xavier Prochaska, Manda Banerji, Xuheng Ding, Masafusa Onoue, Knud Jahnke

Instrumentation and Methods for Astrophysics

Geomagnetic storm suppression of photographic plate transient detections in the POSS-I archive: an independent physical variable strengthening the nuclear test correlation

Kevin Cann

Bruehl & Villarroel (2025) reported a correlation (p = 0.008, 2.6 sigma) between atmospheric nuclear weapon tests and photographic plate transient detection rates in the Palomar Observatory Sky Survey (POSS-I) archive, independently replicated by Doherty (2026) using negative binomial regression with weather controls. I identify geomagnetic storm activity, measured by the planetary Kp index, as an additional independent variable modulating transient rates in the same dataset. Transient detection rates follow a monotonic dose-response across five Kp intensity bins, from 17.4% during geomagnetically quiet periods to 2.4% at Kp 8-9 (Cochran-Armitage trend: Z = -3.391, p = 0.0007). Nuclear test days are not geomagnetically quieter than the baseline; they are slightly more storm-influenced. A multivariate logistic regression including Kp and lunar-phase controls strengthens the nuclear-transient correlation from 2.6 sigma (p = 0.009, OR = 1.53) to 3.1 sigma (p = 0.002, OR = 1.70). The dose-response rules out emulsion defects and spectrally inert orbital debris as the primary transient source, indicating a population physically coupled to the radiation belt environment at geosynchronous altitude. A self-contained reproduction script is provided as supplementary material.
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Astrophysics of Galaxies

Extreme Values of Black Hole to Stellar Mass Ratio for High-Redshift Galaxies

Cameron Heather, Teeraparb Chantavat, Siri Chongchitnan et al. (+1 more)

With recent data from the James Webb Space Telescope (JWST), it is possible to calculate the mass of the supermassive black holes at the center of galaxies, and the stellar mass of the host galaxies at redshift $z \gtrsim 5$. In this work, we apply extreme-value statistics to calculate the distributions of extreme black-hole and stellar masses for galaxies in the redshift range $3 \lesssim z \lesssim 8$. We show that under certain assumptions about the stellar and black-hole mass functions, a high ratio of $M_\text{BH}/M_*\sim0.3-0.5$ can be obtained without invoking additional black-hole growth physics. Nevertheless, surveying a range of extreme-value methodologies, we find predictions of the extreme ratio $M_\text{BH}/M_*$ to still be in slight tension with the high values observed by JWST.
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All authors Cameron Heather, Teeraparb Chantavat, Siri Chongchitnan, Joseph Silk

Astrophysics of Galaxies

The inner dark-matter structure of TNG50 simulated galaxies

Vicente Honorato, Antonio D. Montero-Dorta, M. Celeste Artale et al. (+1 more)

In the $\Lambda$CDM framework, galaxies evolve within dark matter (DM) haloes, where baryonic processes can modify the inner structure of the DM distribution. In particular, the condensation of baryons and associated feedback mechanisms can alter the inner density profiles of haloes, motivating detailed studies of their central regions. We investigate inner DM density slopes in TNG50 galaxies, their relation to galaxy properties, and their cosmic evolution. We assess baryonic effects on the inner DM structure by comparing galaxies with their DM-only (DMO) counterparts. We constructed spherically averaged DM density profiles in both runs. The inner slope was quantified using an inner linear fit, defined as a direct power-law fit to the central region of the density profiles and motivated by the asymptotic behaviour of generalised Navarro-Frenk-White models. Subhaloes were matched between simulations and tracked across redshifts $z = 0$, $0.2$, $0.7$, and $1$. The inner DM structure of galaxies in TNG50 shows that high-stellar-mass systems ($M_\star \gtrsim 10^{11}$ M$_\odot$) exhibit shallow inner slopes regardless of whether they are centrals or satellites, while lower-mass galaxies ($M_\star \lesssim 10^9$ M$_\odot$) show a broader diversity of profiles. At fixed stellar mass, low-mass satellites tend to be more cuspy, with the steepest slopes found in redder systems with lower $V_{\mathrm{max}}$ in more massive host haloes. At the population level, we find a modest cosmic evolution, with steeper profiles towards low redshifts in the hydrodynamical run and the opposite trend in DMO, while hydrodynamical galaxies remain systematically steeper at all redshifts. Finally, we verified that the fiducial interval provides the most suitable reference for measuring the shallowest inner slopes of DM density profiles at the TNG50 resolution limit.
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All authors Vicente Honorato, Antonio D. Montero-Dorta, M. Celeste Artale, Ankit Kumar

Astrophysics of Galaxies

The South Pole Telescope AGN Monitoring Campaign: First Release of SPTpol Bright AGN Light Curves

J. C. Hood II, P. A. R. Ade, A. J. Anderson et al. (+66 more)

The South Pole Telescope (SPT) collaboration has recently embarked upon a campaign to monitor the brightness of a sample of active galactic nuclei (AGN), both in real time and in archival SPT data. The original design of the SPT was optimized for observations of the cosmic microwave background (CMB) at arc-minute and larger angular scales, and it has been used for this purpose for nearly twenty years, using three generations of CMB cameras. Recently it has been recognized that data from CMB experiments have the potential to be used for AGN monitoring. In this paper, we present the first public release of data from a full sample of SPT-monitored AGN, comprising 158 AGN light curves and associated data from the SPTpol camera, which was operational from 2012-2016. These light curves were created using observations from the SPTpol 500 deg$^{2}$ survey, in which the instrument was used to scan a 500 deg$^2$ patch of the sky several times per day with detectors sensitive to radiation in bands centered at 90 and 150 GHz. We provide a comprehensive description of the observations, the data processing methods, and the resulting light curve catalog. As an example of analyses that these data enable, we searched for a correlation between variability and spectral index, and we looked for “bluer-when-brighter” trends in the sample. Our analysis finds $> 10 \sigma$ correlation between fractional intrinsic variance and mean spectral index in the sample, but no significant evidence for bluer-when-brighter trends. The datasets from this study can be accessed through the SPT Treasury Record of AGN With Historical Activity and Time-Series or STRAWHAT catalog. This initial data release includes SPTpol light curves at 90 and 150 GHz, focusing on total intensity. In later updates, SPTpol polarization data and new observations from the SPT-3G instrument at 90, 150, and 220 GHz will be included.
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All authors J. C. Hood II, P. A. R. Ade, A. J. Anderson, M. Archipley, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, J. E. Carlstrom, C. L. Chang, P. Chaubal, H. C. Chiang, T-L. Chou, R. Citron, C. Corbett Moran, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, W. Everett, A. Foster, J. Gallicchio, E. M. George, N. Gupta, N. W. Halverson, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, E. Jarvela, L. Knox, A. T. Lee, D. Li, A. Lowitz, T. J. Maccarone, M. Malkan, J. J. McMahon, S. S. Meyer, J. Montgomery, T. Natoli, J. P. Nibarger, G. Noble, V. Novosad, S. Padin, S. Patil, K. A. Phadke, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, K. K. Schaffer, C. Sievers, A. Simpson, G. Smecher, A. A. Stark, C. Tandoi, C. Tucker, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, J. A. Zebrowski

Instrumentation and Methods for Astrophysics

Speed-Error Cross-Correlation Dating of Ancient Star Catalogues, with Application to the Almagest

Carlos Baiget Orts

We present SESCC (Speed-Error Signals Cross-Correlation), a method for dating ancient star catalogues from the cross-correlation between stellar proper-motion speeds and positional residuals. At the true epoch, residuals are independent of proper-motion speed; the epoch estimate is the trial date that minimises this cross-correlation. For ecliptic latitudes, SESCC applies the dot product between speeds and residuals across all catalogue stars without subset selection or linear modelling. For ecliptic longitudes, SESCC-pairs uses pairwise longitude differences between neighbouring stars, making the method immune to any global longitude offset by algebraic construction. Validated against Tycho Brahe (1547 CE, true ~1580 CE) and Ulugh Beg (1452 CE, true 1437 CE), and confirmed invariant under offsets of +-6 deg, the method is applied to the Almagest. Both coordinates yield bootstrap distributions with 74% pre-Christian minima, consistent with a Hipparchan origin and inconsistent with a Ptolemaic one. The near-absence of quarter-degree fractions in the Almagest longitudes, explained as the deterministic consequence of Ptolemy's precession correction, provides independent corroboration.
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Cosmology and Nongalactic Astrophysics

Return to the Great Attractor: Strong Evidence for a Steradian-sized Flow Converging at $\sim$70 Mpc within the GA Supercluster and Aligned with the CMB Dipole

Alan Dressler and Andrew Monson

We used the FourStar near-IR camera on Magellan-Baade to obtain high S/N H-Band imaging of 66 galaxies with radial velocities of 2000 < V < 5000 km/s. Our goal was to use the superior distance measurements of surface-brightness-fluctuations (SBF) to derive “peculiar velocities” to test claims that the CMB dipole anisotropy, equivalent to $\approx$600 km/s with respect to the Local Group, arises from a 'local' overdensity in the galaxy/dark-matter distribution – the Great Attractor. SBF's ability to measure distances with 5% accuracy confirms a strong flow over a steradian of the sky peaking at Vpec $\sim$ 1000 km/s and converging to zero at D $\approx$70 Mpc from the Local Group. The modest spatial extent of this flow $R_V$ $\sim$ 5000 km/s is consistent with the original Great Attractor model (a diameter D $\sim$ 140 Mpc), as well as the magnitude and direction of the CMB dipole anisotropy, and the power spectrum of CMB fluctuations – the latter two arguably the most secure measurements in astrophysics. In contrast, our results are at-odds with reports of comparable amplitude 'bulk flows' on scales of hundreds of Mpc that themselves may be inconsistent with the expected fluctuations in the CMB for a $\Lambda$CDM universe. We contend that only distance-estimators as accurate as SBF are able settle the question of whether the CMB dipole arises from the gravitational influence of large-scale structure within, or without $\sim$100 Mpc of the Local Group.
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Earth and Planetary Astrophysics · Cross-listed from math.DS

Effective Stability of Near-Rectilinear Halo Orbits in the Earth-Moon System

Joan Gimeno and Luke T. Peterson

Near-rectilinear halo orbits (NRHOs) around Earth-Moon L2 in the Circular Restricted 3-Body Problem (CR3BP) exhibit a complex dynamical landscape, featuring a band of normally elliptic orbits embedded within regions of strong instability. This coexistence of stable and unstable dynamics, amplified by the numerical sensitivity associated with close lunar passages, makes the long-term behavior of trajectories near NRHOs a delicate and intrinsically nonlinear problem. Understanding the effective stability of these elliptic orbits is therefore a critical challenge, lying at the intersection of local normal form theory and global instability mechanisms. To quantify finite-time confinement, we formulate a rigorous framework for effective stability using discrete Poincaré maps. By employing jet transport to compute high-order Taylor expansions, we construct explicit polynomial normal forms. We derive discrete Nekhoroshev-type estimates by identifying the normalization order, which balances the asymptotic convergence of the map's analyticity domain against the cumulative penalty of low-order small divisors. Applying this framework to the Earth-Moon system, we map the resulting geometric limits directly into physical spatial coordinates. Crucially, we demonstrate that for practical mission lifetimes (e.g., 10-50 years), the required stability is vastly shorter than the characteristic Nekhoroshev accumulation time. Consequently, the effective stability region is not constrained by the time-dependent exponential drift, but is instead governed entirely by the maximum analytical domain of the optimized normal form. These derived spatial envelopes establish explicit geometric boundaries for the intrinsic local stability of elliptic NRHOs, providing a rigorous mathematical characterization of their nonlinear confinement within the CR3BP.
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Astrophysics of Galaxies

Cosmic-web quenching with DESI DR1: T-Web environments and mass-dependent red/blue classification

Hafiz Inam Ullah, Muhammad Awais, Tonatiuh Matosb et al. (+1 more)

We study DESI DR1 galaxies to quantify colour dependence on cosmic web environment for three tracers spanning complementary regimes: BGS ($0.15\le z<0.55$), LRG ($0.6\le z<0.9$), and ELG ($0.6\le z<1.6$). Web environments are reconstructed with the tidal-tensor (T-Web) formalism on a $256^3$ grid in an $800\,Mpc$ cube and classified into voids, sheets, filaments, and knots. Sheets and filaments dominate volume ($\sim 45$–$48\%$ and $\sim 37$–$40\%$), voids $\sim 6$–$16\%$ knots $\sim 4$–$6\%$. A mass-dependent Otsu method separates red and blue populations. The BGS red fraction evolves non-monotonically: at $z\approx0.20$, voids ($13.89\pm5.76\%$), sheets ($6.13\pm1.27\%$), filaments ($9.24\pm1.66\%$), knots ($6.12\pm3.42\%$); at $z\approx0.30$, values range from $0.63\pm0.44\%$ to $2.01\pm0.99\%$; at $z\approx0.50$, from $17.93\pm0.44\%$ to $19.63\pm1.08\%$; environmental differences are small. LRGs show environment-dependent quenching: at $z\approx0.66$, knots ($65.90\pm0.45\%$), voids ($62.40\pm1.81\%$), filaments ($60.21\pm0.48\%$), sheets ($58.37\pm3.15\%$); by $z\approx0.88$, these converge to $\sim 68$–$70\%$. ELGs exhibit strong redshift evolution: filaments drop from $55.18\pm0.31\%$ at $z\approx0.65$ to $33.22\pm0.21\%$ at $z\approx0.95$; voids and sheets show similar declines, with weak and non-monotonic. High-mass selection increases red fractions but preserves trends. Relative red and blue fractions (RRF/RBF) show filaments and sheets host the largest shares of both red and blue galaxies; knots contribute less despite elevated red fractions. The $(g-r)$ colour distributions reveal an enhanced red component in knots and bluer colours in voids, with the clearest bimodality at low redshift. Overall, stellar mass drives the primary quenching trend, while environment provides a systematic secondary modulation, strongest in dense knots and at lower stellar masses.
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All authors Hafiz Inam Ullah, Muhammad Awais, Tonatiuh Matosb, John F. Suárez-Pérez

Earth and Planetary Astrophysics · Cross-listed from physics.space-ph

Proton Temperature Anisotropy Across Interplanetary Shocks: A Statistical Analysis with WIND observations

Zeping Jin, Lingling Zhao, Xingyu Zhu et al. (+6 more)

Interplanetary (IP) shocks efficiently modify the proton temperature anisotropy of the solar wind. Analyzing ~800 IP shocks observed by the Wind spacecraft from 1997-2024, we present a statistical study of upstream and downstream proton temperature anisotropy and its dependence on shock geometry, compression, and distance from the shock. We find that (1) quasi-perpendicular shocks produce a pronounced enhancement of perpendicular temperature downstream (Tperp > Tpara), whereas parallel shocks remain near isotropic downstream due to typically stronger upstream Tpara; (2) comparisons with the Chew-Goldberger-Low (CGL) double-adiabatic model reveal geometry-dependent deviations. CGL overestimates downstream perpendicular heating and underestimates parallel heating at quasi-perpendicular shocks, with the opposite trend at quasi-parallel shocks, highlighting the importance of non-adiabatic processes beyond simple compression; (3) Shock-driven anisotropy is strongly localized near the shock and gradually relaxes toward typical solar wind conditions farther downstream as the shock's influence diminishes; and (4) downstream anisotropy is regulated by kinetic instabilities, with quasi-perpendicular shocks constrained by proton cyclotron and mirror instabilities and quasi-parallel shocks limited by the parallel firehose instability. Together, these results show that the evolution of temperature anisotropy at interplanetary shocks is controlled by shock geometry, localized processes, and instability driven regulation.
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All authors Zeping Jin, Lingling Zhao, Xingyu Zhu, Vladimir Flosinski, Gary P. Zank, Jakobus Le Roux, Yiming Jiao, Ashok Silwal, Nibuna S. M. Subashchandar

High Energy Astrophysical Phenomena · Cross-listed from gr-qc

Exact general relativistic solutions for a cylindrically symmetric stiff fluid matter source

Tiberiu Harko, Francisco S. N. Lobo and Man Kwong Mak

In this work, we derive the general solutions for a cylindrically symmetric space-time filled with a cosmological perfect fluid obeying $p=\gamma \rho$ ($0\leq \gamma \leq 1$), where $\gamma=1$ represents a stiff or Zeldovich fluid. Using Marder's metric with coefficients depending on $t$ and $r$, we obtain explicit solutions of the gravitational field equations for the three cases $\delta = 1, 0, -1$, corresponding to exponential, power-law, and trigonometric behaviors of the metric functions. The resulting space-times exhibit anisotropic evolution, nontrivial expansion and shear, and curvature singularities, with energy density and pressure profiles determined by the integration constants. These solutions provide a comprehensive framework for modeling cylindrically symmetric cosmologies, offering insights into early-universe dynamics and anisotropic gravitational phenomena. The versatility of the solutions also opens avenues for extensions to higher-dimensional or modified gravity scenarios, making them a valuable tool for both theoretical and phenomenological studies in general relativity.
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Instrumentation and Methods for Astrophysics

PLATO input catalogs for technical calibration and fine guidance

René Heller, Chen Jiang, Paz Bluhm et al. (+18 more)

A few weeks after launch, the PLATO spacecraft is expected to start its payload commissioning, which will be completed within the first three months of the mission. This phase includes the in-orbit verification, calibration, and configuration of the instrument prior to nominal science operations. During this mission-critical period, and again later during regular spacecraft rotations and re-pointings, a set of reference stars is required to complete various calibration steps. This set, referred to as the calibration PLATO Input Catalog (cPIC), is part of the PIC. The cPIC comprises various stellar samples, each serving a dedicated technical calibration purpose, and it contains 71671 unique stellar targets across PLATO's entire field of view (FoV). Once the spacecraft commences science observations, the on-board Fine Guidance System (FGS) will rely on a small set of guide stars. These stars must be particularly bright and will be observed with the two fast cameras, which cover only a smaller central region of PLATO's FoV. This target list, referred to as the fine-guidance PLATO Input Catalog (fgPIC), contains 2640 unique targets, of which about 30 are used by the FGS at any given time. In this paper, we present the selection criteria for both the cPIC and the fgPIC, and asses their impact on the construction of these calibration catalogs for PLATO.
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All authors René Heller, Chen Jiang, Paz Bluhm, Valentina Granata, Juan Cabrera, Denis Grießbach, Carsten Paproth, Szilárd Csizmadia, Philipp Eigmüller, Paola Maria Marrese, Silvia Marinoni, Réza Samadi, Giampaolo Piotto, Marco Montalto, Martin Schäfer, Cilia Damiani, Nicholas Walton, Christoph Rauterberg, Matthias Ammler-von Eiff, Aaron C. Birch, Laurent Gizon

Cosmology and Nongalactic Astrophysics

Cosmology-Independent Constraints on the Etherington Relation and SNeIa Absolute Magnitude Evolution from DESI-DR2

Sourav Das, Surhud More and Shadab Alam

We carry out a test of the fundamental Etherington relation (cosmic distance duality relation) which relates the luminosity distance $D_{\rm L}$ and angular diameter distance $D_{\rm A}$ in metric theories of gravity. We use the latest measurements of the angular diameter distance as a function of redshift from the Dark Energy Spectroscopic Instrument Data Release 2 (DESI-DR2) and the luminosity distance from a variety of compilations of Supernovae of Type Ia (SNeIa). Our results indicate that these measurements are statistically consistent with the Etherington relation. In addition to providing a confirmation of the underlying assumptions of the Etherington relation, i.e., the metric nature of gravity, Lorentz invariance and photon number conservation, our results are also a stringent test of any residual systematic effects. We interpret the absence of evidence of any deviation from this relation to constrain the evolution of the absolute magnitude of SNeIa to $dM/dz = 0.07 \pm 0.07$ over and above the systematics that are already accounted for in the SNeIa analyses. We discuss how the Etherington relation can be used to constrain systematic parameters in the analyses of dynamical dark energy using geometric probes, to make it more robust against systematic effects.
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Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph

Imprint of matter-antimatter asymmetry on collapsing domain walls

Dipendu Bhandari, Debasish Borah and Indrajit Saha

Spontaneous breaking of discrete symmetries play non-trivial role in many well-motivated particle physics models. However, it leads to a network of cosmologically unwanted domain walls (DWs) which can be made unstable by introducing a bias term in the scalar potential. In this letter, we provide a novel origin of such bias terms at finite temperature due to radiative corrections from a Dirac fermion with large asymmetry $\sim \mathcal{O}(0.1)$ in its number density. In addition to getting a new viable region of parameter space for collapsing DWs not explored previously and resulting gravitational waves (GWs) accessible at future experiments, the viability of the scenario crucially depends on the temperature of asymmetry generation too. This provides a unique way of probing both the amount of asymmetry and the corresponding temperature via future observations of GWs from collapsing DWs. The large asymmetry in the Dirac fermion can also have interesting implications for the observed baryon asymmetry as well as dark matter and large neutrino asymmetry.
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Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph

Millicharged Particle Production During Late-Stage Stellar Evolution

Damiano F. G. Fiorillo, Giuseppe Lucente, Jeremy Sakstein et al. (+1 more)

Stars are natural sources of feebly interacting particles, including putative particles with mass $m_\chi$ and electric charge $qe$. The emission of such millicharged particles (MCPs) causes an energy loss which can alter stellar evolution. While MCP production rates have been computed for different plasma parameters, they have yet to be derived for the conditions relevant to late stages of stellar evolution, in which the temperature can reach values $T\simeq 10-100\,\rm keV$ while the plasma frequency is $\omega_{\rm pl}\ll T$. In this paper, we compute the MCP energy-loss rates relevant for pre-supernova objects, finding three different regimes in which the dominant processes are respectively plasmon decay ($m_\chi< \omega_{\rm pl}/2$), Compton-like scattering ($m_\chi> \omega_{\rm pl}/2$, $T\lesssim 0.5\,\rm MeV$), and electron-positron annihilation. We obtain semi-analytical fits for the energy-loss rates suitable for implementation in stellar evolution codes.
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All authors Damiano F. G. Fiorillo, Giuseppe Lucente, Jeremy Sakstein, Edoardo Vitagliano

Astrophysics of Galaxies

Supernova 2025wny: High-angular resolution Keck/NIRC2 observations and preliminary lens modeling

Christopher J. Storfer, Kenneth C. Wong, Ana Acebron et al. (+10 more)

Multiply imaged, gravitationally lensed supernovae are rare but powerful tools for providing independent measurements on cosmological parameters. Supernova (SN) 2025wny ("SN Winny") is the first gravitationally-lensed Type I superluminous supernova and the first lensed supernova in a galaxy-scale system that is suitable for time-delay cosmography studies. In this work, we present high-resolution $K_p$-band adaptive optics imaging of SN Winny obtained with the near-infrared camera (NIRC2) on the W. M. Keck II telescope. With exquisite image quality (FWHM$\approx0.^{\prime\prime}065$) we determine and make use of the precise astrometric positions of the five multiple images as constraints for our lens mass models. With lenstronomy and Glee, we parameterize the total mass of the system with a singular isothermal ellipsoid, a singular isothermal sphere, and external shear. The two independent models are in excellent agreement and reproduce the observed image positions with sub-milli-arcsecond residuals. The inferred projected total masses enclosed within the Einstein radii of the primary and secondary lens galaxies are M$_1$ = 4.44$^{+0.06}_{-0.05}\times10^{11} M_\odot$ and M$_2$ = 0.96$^{+0.02}_{-0.02}\times10^{11} M_\odot$, respectively. Likewise, the inferred effective velocity dispersion of the primary lens is $\sigma_{1} = $ 277.4$^{+0.9}_{-0.7}$ km/s, consistent with the independent spectroscopic measurement made by DESI of $\sigma_{\star,1} = $ 298$\,\pm\,37$ km/s. Our modeling results are also consistent with previous results for the same system with data from the Large Binocular Telescope (LBT), using the same lens modeling codes. We also corroborate their finding that the SN multiple image A has an anomalous excess of flux by a factor of ~2-3 beyond what our smooth mass models predict.
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All authors Christopher J. Storfer, Kenneth C. Wong, Ana Acebron, Claudio Grillo, Willem B. Hoogendam, Xiaosheng Huang, David O. Jones, Eugene A. Magnier, Kaisey S. Mandel, Nicolas Ratier-Werbin, David Rubin, Benjamin J. Shappee, Oscar Soler-Perez

Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph

The Black Hole Mass Gap as a New Probe of Millicharged Particles

Damiano F. G. Fiorillo, Giuseppe Lucente, Jeremy Sakstein et al. (+2 more)

We investigate the impact of millicharged particles (MCPs) on massive stars undergoing pulsational pair-instability supernovae and on the location of the lower edge of the black hole mass gap. We find that energy losses due to MCP emission weaken the pulsations, allowing the star to retain more mass and thereby shifting the lower edge of the mass gap to higher black hole masses. The mass gap is sensitive to a region of MCP parameter space with masses $35\,{\rm keV}\lesssim m_\chi \lesssim 200\,{\rm keV}$ and charges $10^{-10}\lesssim q \lesssim 10^{-9}$, which remains unconstrained by existing astrophysical probes. If confirmed, recent gravitational wave observations placing the lower edge of the mass gap near $45\,{\rm M}_\odot$ would translate directly into bounds on this parameter space.
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All authors Damiano F. G. Fiorillo, Giuseppe Lucente, Jeremy Sakstein, Edoardo Vitagliano, Matteo Cantiello

Astrophysics of Galaxies

An analytical approach to binary populations in globular clusters

Christopher E. O'Connor, Kyle Kremer and Frederic A. Rasio

Globular clusters (GCs) display much lower binary fractions than found among main-sequence stars in the solar neighborhood. The physical cause of this difference is debatable: does it reflect different star formation outcomes at low metallicity and/or high density, the dynamical processing of primordial binaries over cluster lifetimes, or a combination of the two? Starting from the assumption that the initial binary distribution in GCs is the same as the binary distribution observed in the solar neighborhood, we show with straightforward analytical calculations that the dynamical dissolution of "soft" primordial binaries can fully explain the main-sequence binary fractions in present-day GCs. We validate our estimates against a detailed N-body simulation with the Cluster Monte Carlo code. Adopting the view that the observed binary fraction in a given cluster constrains the location of the hard/soft boundary at birth, we infer that surviving Milky Way GCs had a similar distribution of birth radii to young massive clusters in the local universe. Our findings underscore the crucial role of stellar black holes (through "black hole burning") in sculpting GC binary populations and reinforce the need for realistic initial conditions in theoretical modeling of GC dynamics.
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High Energy Astrophysical Phenomena

A high-resolution study of the double radio relic system in MACS J1752.0+4440

M. Della Chiesa, A. Botteon, A. Bonafede et al. (+6 more)

Radio relics are diffuse, extended synchrotron sources located at the outskirts of merging galaxy clusters. Their origin has been linked with shock waves injected into the intracluster medium, but the acceleration mechanism at the shock front is still under debate. Some clusters, like MACS J1752.0+4440, host a double relic system, with two relics found on opposite sides with respect to the cluster center. To investigate the acceleration mechanism that generates radio relics, we study the morphological and spectral properties of the double relic system in MACS J1752. We present new wideband radio continuum observations made with uGMRT and JVLA, and LOFAR data. We perform a detailed, high-resolution spectral analysis of the double relic system in MACS J1752, observing and characterizing substructures, particularly for the brighter relic. We find a double-peaked surface brightness and spectral index profile for the NE relic and identify a "bright bar" substructure. Moreover, we observed surprisingly flat integrated spectral indices for both relics, at $\alpha_{\mathrm{int}}^{\mathrm{NE}} = -0.91 \pm 0.06$ and $\alpha_{\mathrm{int}}^{\mathrm{SW}} = -0.83 \pm 0.05$. We study the spatial variation of the spectral index, observing a coherent trend with the observed substructures. We estimate an injection Mach number of $\mathcal{M}_{\mathrm{NE}} = 3.1^{+0.1}_{-0.1}$ and $\mathcal{M}_{\mathrm{SW}} = 3.2^{+0.1}_{-0.1}$. By performing a spectral curvature analysis for both relics, generating color-color plots and a spectral curvature maps, we observe two "concave" spectra represented by positive spectral curvature, in contrast with particle population ageing models. The observed properties of the NE relic are not consistent with a simple scenario with a single shock front. Multiple shock surfaces, re-acceleration, and projection effects likely play a role in shaping the morphology of the relic.
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All authors M. Della Chiesa, A. Botteon, A. Bonafede, K. Rajpurohit, V. Cuciti, D. Hoang, R. J. van Weeren, X. Zhang, F. Gastaldello

Instrumentation and Methods for Astrophysics

Site selection for the Laser Interferometer Lunar Antenna (LILA)

James Trippe, Ronald Polidan, Teviet Creighton et al. (+6 more)

The Earth's Moon presents a uniquely advantageous environment for detecting astrophysical gravitational waves (GWs), particularly in the decihertz regime. The Laser Interferometer Lunar Antenna (LILA) project plans to perform GW measurements on the lunar surface, using the Moon's seismic quietness to access this band. Two mission concepts are considered: the proof-of-concept 1 km initial LILA (iLILA) and the full LILA Observatory, whose equilateral arms are at least 40 km long. The Moon's changing orientation and orbital motion provide the time-dependent source modulation needed for sky localization, so the detector response does not impose a unique lunar region. Practical considerations, most critically line of sight (LOS), nevertheless constrain deployment. A coarse-to-fine search of existing lunar datasets identifies and ranks candidate grid locations. Of 4,050 global grid seeds, 434 iLILA seeds and 71 Observatory circumcenters pass both search stages. These results demonstrate that sites suitable for GW detection naturally exist in large numbers on the lunar surface.
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All authors James Trippe, Ronald Polidan, Teviet Creighton, Philippe Lognonné, Mark Panning, Volker Quetschke, Kris Izquierdo, Brett Shapiro, Karan Jani

Earth and Planetary Astrophysics

Hot Rocks Survey V: Secondary Eclipse Photometry of GJ 3473 b with JWST/MIRI

Måns Holmberg, Hannah Diamond-Lowe, João M. Mendonça et al. (+16 more)

JWST is transforming our ability to characterise small exoplanets, from sub-Neptunes to rocky worlds. A key open question is whether highly irradiated rocky planets can retain atmospheres or are stripped bare by stellar irradiation – a boundary that remains to be mapped observationally. Here we present the first JWST secondary eclipse observations of the rocky exoplanet GJ 3473 b, obtained with MIRI F1500W photometry. Using four visits, we confidently detect the eclipse at an average depth of 186$\pm$45 ppm, somewhat lower than expected for a blackbody. We test a wide range of data reduction and analysis assumptions and provide new insights into MIRI detector settling behaviour that will benefit future observations. We model a suite of airless surfaces with varied compositions, textures, and degrees of space weathering, as well as idealised atmospheric scenarios including the possibility of atmospheric collapse. Both atmospheric and bare-rock interpretations remain consistent with the data, but we exclude thick CO$_2$ atmospheres, placing a 95 % credible upper limit of 1.2-6.5 bar on the surface pressure. We also find tentative evidence for visit-to-visit variability in eclipse depth (33-371 ppm), though additional data are required to confirm this. Our results highlight the challenges and intrinsic degeneracies in interpreting MIRI F1500W eclipse measurements of rocky exoplanets, indicating that such observations alone may not uniquely distinguish between bare-rock and atmospheric scenarios. Future spectroscopic or phase-curve observations will be required to determine whether or not GJ 3473 b hosts a substantial atmosphere
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All authors Måns Holmberg, Hannah Diamond-Lowe, João M. Mendonça, Daniel Kitzmann, Néstor Espinoza, Natalie H. Allen, Prune C. August, Mark Fortune, Amélie Gressier, Jegug Ih, Erik Meier Valdés, Merlin Zgraggen, Lars A. Buchhave, Brice-Olivier Demory, Chloe Fisher, Neale P. Gibson, Kevin Heng, Bibiana Prinoth, Adam J. Burgasser