Publications of the Astronomical Society of the Pacific (PASP)

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Publishing original research in astronomy and astrophysics since 1889. Currently led by Editor-in-Chief Jeff Mangum (@jeffreygmangum.bsky.social)

Spectrum of GB6 J010341+423925 with identified lines. From Blinov etal (2026).
Stellar activity cycle period versus rotation period with points colored by effective temperature for stars with these measurements available in the HWO Activity and Rotation Catalog (ARC). From Fetherolf etal (2026).
Forecasting performance of all models trained using a 2 hr input window. Left: RMSE, and Right: Pearson correlation coefficient, both computed between the predicted and observed seeing values and plotted as a function of forecast lead time. From Medlej etal (2026).
The number of objects in Earth orbit over time aggregated from archival three-line elements from Space-Track (United States Space Command 2025). From Miller etal (2026).
Photometric improvement delivered by the RTN correction algorithm for 766 stars observed with QHY600M-C. From Layden etal (2026).
Constraints on main sequence tertiaries to Gaia BH1 from NIRC2-LGS AO imaging (blue, this work), precision radial velocities (RVs, orange) (Nagarajan et al. 2024), and spectral disentangling (red) (El-Badry et al. 2023a). From Nagarajan etal (2026).
Simulated (top) and observed (bottom) fringe patterns from a lateral shearing plate interferometer. From Bernard etal (2026).
An example of a raw (left) and clean (right) TDI ILMT image. From Negi etal (2026).
Corner plot showing the posterior probability distributions and covariances of the orbital parameters (P, T0, e, ω, K1, K2, γ and q) derived. From Barbaros, Ak, and Filiz Ak (2026).
Comparison of average RVs (left panel) and RV dispersion (right panel) derived from singles, binaries, and red clump giants with those derived from member stars. From Tang etal (2026).
Distance-free log(L_hX/L_y) ratio diagnostic. From Kun etal (2026).
Analysis of Milky Way inner halo structures. From Akbaba & Plevne (2026).
Radial intensity profiles of the long-exposure PSF for HAWK-I+GRAAL under good seeing (ε0≈0.″45; left) and median seeing (ε0≈0.″70; right), from the on-axis MAAO simulation. From Guzman etal (2026).
OGLE light curve for AzV 493 at I (black) and V (red) bands. From Oey etal (2026).
Distribution of proposal rank spreads in Stage 1 and Stage 2 of DPR for Cycles 8–12. From Carpenter etal (2026).
Example pipeline finding chart product for the transient candidate AT 2025ifl. From Hu etal (2026).
Model architecture for RuBR (Rotational Invariant CNN with Feature encoder). From Gandhi etal (2026).
Example of the nebular spectral analysis procedure for ZTF22abtjefa/SN 2022aaad at phase 332days. From Das etal (2026).
Two prototypes of modules from MPS (left) and Orbray (right) captured at LBNL for the project Spec-S5 (Besuner et al. 2025). From Galal etal (2026).
Stacked histogram of the evolution of the number of ALMA publications per year. From Stoehr etal (2026).
Schematic of the fiber assignment problem. Left: physical focal plane with overlapping patrol areas; targets at intersections are accessible to multiple RFPs. Right: corresponding constraint graph. From Cui etal (2026).
The magnitude–period two-dimensional distribution of asteroids with reliable rotation periods derived in this work, compared with those from the LCDB-BASIC (Warner et al. 2009). The gray dashed line indicates the asteroid spin barrier at ∼2.2 hr. From Huang etal (2026).
Schematic illustration of nonlinear magnetothermal drip in a stratified atmosphere with a uniform horizontal magnetic field of strength B0. From Voit, Wibking, and Yaldiz (2026).
Cumulative distributions of PWV and 225 GHz opacity monitored by the radiometer at the Ali observatory. From Qian etal (2026).
Recovered images under three sampling fronts using the same interference cancellation and imaging framework: (a) an ideal sampler, (b) a conventional finite-dynamic-range sampler, and (c) the proposed modulo-sampling-enabled RI front-end. From Ahmed, Zeng, & Li (2026).
Measured spectra from 8 signals from the OVRO-LWA, after equalization and re-quantization, used in the analysis. From Byrne etal (2026).
Density maps in three Cartesian planes for CCSN G11.2-0.3. From Akashi & Soker (2026).
The morphology distribution of 14,288 ALFALFA sources with respect to the MH I, colors and concentration indices. For each plot the Pearson correlation coefficient is given. From Janak etal (2026).
Vertical and midplane slices of the GRMHD snapshot from the models presented. From Thomas etal (2026).
Functional spectral reconstruction of the Neptune Trojan 2010 TS191 across the informational hierarchy. From Lin & Sie (2026).
Example results from the morphology analysis algorithm presented. From Xie et al. (2026).
LAMOST fiber positioner analysis results. From Yang etal (2026).
Example images from DESI Legacy Imaging Surveys. CV stars are located at the center of each image. From Cao, Jiang & Zhang (2026).
Example of the implementation of the TI symmetry identifier for the PN M1-37. From Shishkin & Michaelis (2026).
The average velocity of flow versus pressure, pb, when the macro porosity is ψd = 0.43. From Kossacki, Wesolowski & Szutowicz (2026).
Companion mass distribution for the full sample of 57 brown dwarf companions. From Karamiqucham (2026).
Comparison of 10″× 10″near-infrared cutouts centered on the radio localization of PSR J1928+1815 from the UKIDSS survey (left), the EMIR program of Gong et al. (2025), and NIRC2 campaign measurements from this article (right). In both the UKIDSS cutout and the NIRC2 image, the position of the pulsar is marked with a red circle. From Nagarajan etal (2026).
An analysis of mass segregation in the fifteen open clusters analyzed. From Alfonso, Garcia-Varela & Vieira (2026).
Historical photometric light curve of V854 Cen (R Coronae Borealis star) spanning 1890 to 2026. From Zafar & Hudec (2026).
Three representations of the Gaia Phase Spiral from Antoja etal (2018).
Sunspot number prediction forecast for SC25 and SC26 base on the model presented. From Ye etal (2026).
Example of a PSF-like alpha-cluster detected in only one of two consecutive 30 second exposures obtained on 2025 May 29. From Megias Homar etal (2026).
Habitable zone and planetary orbits in the HD 20794 planetary system. From Kane (2026).
All-sky density distribution of the Gaia DR3 sample (N=1,742,306). From Torlakcik (2026).
Example flare detection and envelope expansion from AD Leo. From Bertollini (2026).
Sample spectra output from the RFI monitor showing a measured system sensitivity of ≈ −172 dBm Hz−1, aligning with the theoretical prediction (red dashed line) of Sx = −172.7 Bm Hz−1. From Bruce etal (2026). .
Cost-effectiveness ratio of a diffraction-limited telescope array (element diameter Da) relative to a diffraction-limited single telescope of diameter D1 at equal survey speed. From Ben-Ami and Ofek (2026).
Flowchart for BOOM. From Jegou du Laz etal (2026).
Mean squared error calculated between the true and CVAE-generated physical parameters for chirp mass, mass ratio, fraction of the remnant disk and viewing angle while grouped according to the filter bands. From Saha & Kong (2026).
Integration time required to detect an Earth-twin around a given star to a SNR of 7, plotted as a function of stellar parameters. From Hansen etal (2026).
Sample atmospheric transmission profiles. From Qiu etal (2026).
Representative samples of the six density classes used in the described classification algorithm. From Lai etal (2026).
proto-Lightspeed (left and middle) and HST (right) images of the quadruply-lensed quasar DES J0420-4037 and its lensing galaxy. From Layden etal (2026).
Architecture of the spectrum encoder based on masked modeling from Dong etal (2026).
Transmission curves of the individual components contributing to the proto-NUX system throughput. From Sloot etal (2026).
Graphical representation of AppleCiDEr's role in the planned ZTF production pipeline. From Junell etal (2026).
Class-conditional distributions of selected planetary and stellar parameters in the final data set. From El-Kholy & Hayman (2026).
Example supernova remnant images, showing radio (left), smoothed x-ray (center), and unsmoothed x-ray (right) images used in this analysis. From Leahy etal (2026).
Color-magnitude diagram of the LSP samples used in this work. From Shariat etal (2026).
Photo of the current 256-antenna main BURSTT array in Fushan. From Lin etal (2026).