============================================================================== Lyman Alpha Nebulae in HETDEX: The Largest Statistical Census Bridging Ly-alpha Halos and Blobs Across Cosmic Noon ============================================================================== Catalog file: hetdex_lan_v0.3.fits This catalog accompanies the paper: Mentuch Cooper, E., et al. "Lyman Alpha Nebulae in HETDEX: The Largest Statistical Census Bridging Ly-alpha Halos and Blobs Across Cosmic Noon" DOI: https://doi.org/10.3847/1538-4357/ae44f3 ------------------------------------------------------------------------------ Description: This catalog presents a uniformly selected sample of Lyman-α nebulae identified in the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX). The sample provides the largest statistical census to date of extended Lyman-α emission during cosmic noon (approximately 10–11 billion years ago), bridging the population of galaxy-scale Lyman-α halos and the most extended Lyman-α blobs. Each row corresponds to a single HETDEX Lyman-α Nebula (HLAN). Multiple rows exist for repeat observations of the same object. Use column dups_detectid to locate repeat LANs. ------------------------------------------------------------------------------ Table: hetdex_lan_v0.3.fits Column descriptions: ------------------------------------------------------------------------------ name (char[14]) Unique HETDEX Lyman-Alpha Nebula identifier, constructed as 'HLAN+' followed by the HETDEX detectid. ra (float32) Right ascension of the nebula centroid (ICRS). dec (float32) Declination of the nebula centroid (ICRS). source_type (char[10]) Source classification based on HETDEX catalog cross-matching. Typical values are 'lae' (Lyman-α emitter) and 'agn' (active galactic nucleus). z_hetdex (float32) Spectroscopic redshift measured by HETDEX. z_hetdex_src (char[8]) Identifier describing the source of the redshift measurement. detectid (int64) Unique HETDEX detection identifier. shotid (int64) HETDEX observation (shot) identifier. field (char[12]) HETDEX survey field name. SB_1sigma_obs (float32) Observed-frame 1σ Lyman-α surface-brightness sensitivity per IFU exposure, in units of 1e-18 erg s^-1 cm^-2 arcsec^-2. r_iso (float32) Isophotal radius defined as the circular aperture radius at which the Lyman-α surface brightness falls below the 1σ sky background level. Reported in proper kiloparsecs. r_s (float32) Exponential scale length of the nebular surface-brightness profile, in proper kiloparsecs. r_s_err (float32) 1σ uncertainty on r_s. area_iso_2sigma (float32) Isophotal sky area above a 2σ surface-brightness threshold, in arcsec^2. area_r_iso_circ (float32) Circular isophotal area corresponding to r_iso. logL_lya (float32) Log10 of the Lyman-α luminosity. logL_lya_err (float32) Uncertainty on logL_lya. flux_lya (float32) Integrated Lyman-α flux. flux_lya_err (float32) Uncertainty on the integrated Lyman-α flux. gmag (float32) g-band magnitude from ancillary imaging. HSC-r_mag (float32) r-band magnitude from Hyper Suprime-Cam (HSC) imaging. HSC-r_mag_err (float32) Uncertainty on the HSC r-band magnitude. combined_eqw_rest_lya (float32) Rest-frame Lyman-α equivalent width measured from combined spectral data. flag_resolved (int64) Flag indicating whether the source is spatially resolved relative to the point-spread function. chi2_ext_reduced (float32) Reduced χ² value for the extended-source model fit. chi2_psf_reduced (float32) Reduced χ² value for the point-source (PSF) model fit. log10_pF (float32) Log10 probability favoring the extended-source model over the PSF model. dBIC (float32) Difference in Bayesian Information Criterion between extended and PSF models. iso_rel_err (float32) Relative uncertainty on the isophotal radius. dups_detectid (char[60]) Identifier indicating duplicated detections associated with the same astrophysical source. ------------------------------------------------------------------------------ Notes: (1) The catalog contains uniformly selected Lyman-α Nebulae (LANs) identified in the HETDEX IFU survey. Each row corresponds to one nebula associated with a unique HETDEX detection. There can be multiple rows corresponding to multiple observations of the same astrophysical source. (2) Source classifications and redshifts are spectroscopic and derived following the methodology of Davis et al. (2023), as described in Mentuch Cooper et al. (2023). (3) Physical sizes are given in proper kiloparsecs assuming the Planck 2018 cosmology adopted in the paper. (4) Isophotal quantities depend on surface-brightness sensitivity and should not be interpreted as total nebular extents. ------------------------------------------------------------------------------ References: Mentuch Cooper, E., et al., 2023, ApJ, 943, 177 Davis, D., et al., 2023, ApJ, 946, 86 Mentuch Cooper, E., et al., 2026, ApJ, 1000, 38 ------------------------------------------------------------------------------ Acknowledgements: HETDEX is led by the University of Texas at Austin McDonald Observatory and Department of Astronomy with participation from the Ludwig-Maximilians- Universität München, Max-Planck-Institut für Extraterrestrische Physik (MPE), Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Pennsylvania State University, Institut für Astrophysik Göttingen, the University of Oxford, Max-Planck-Institut für Astrophysik (MPA), the University of Tokyo, and Missouri University of Science and Technology. Observations for HETDEX were obtained with the Hobby-Eberly Telescope (HET), which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Visible Integral-field Replicable Unit Spectrograph (VIRUS) was used for HETDEX observations. VIRUS is a joint project of the University of Texas at Austin, Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Max-Planck-Institut für Extraterrestrische Physik (MPE), Ludwig-Maximilians-Universität München, Pennsylvania State University, Institut für Astrophysik Göttingen, the University of Oxford, and the Max-Planck-Institut für Astrophysik (MPA). The authors acknowledge the Texas Advanced Computing Center (TACC) at the University of Texas at Austin for providing high-performance computing, visualization, and storage resources that have contributed to the research results reported in this paper (http://www.tacc.utexas.edu). Funding for HETDEX has been provided by the partner institutions, the National Science Foundation, the State of Texas, the U.S. Air Force, and by generous support from private individuals and foundations. ==============================================================================