124 research outputs found

    CWITools: A Python3 Data Analysis Pipeline for the Cosmic Web Imager Instruments

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    The Palomar Cosmic Web Imager (PCWI) and Keck Cosmic Web Imager (KCWI) are integral-field spectrographs on the Hale 5m telescope at Palomar Observatory and the Keck-2 10m telescope at W. M. Keck Observatory, respectively. In recent years, these instruments have been increasingly used to conduct survey work; in particular focused on the circumgalactic and intergalactic media at high redshift. Extracting faint signals from three-dimensional IFU data is a complex task which can become prohibitively difficult for large samples without the proper tools. We present CWITools, a package written in Python3 for the analysis of PCWI and KCWI data. CWITools is designed to provide a pipeline between the output of the standard instrument data reduction pipelines and scientific products such as surface brightness maps, spectra, velocity maps, as well as a wide array of associated models and measurements. While the package is designed specifically for PCWI and KCWI data, the package is open source and can be adapted to accommodate any three-dimensional integral field spectroscopy data. Here, we describe this pipeline, the methodology behind individual steps and provide example applications

    The FLASHES Survey I: Integral Field Spectroscopy of the CGM around 48 z=2.3−3.1z=2.3-3.1 QSOs

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    We present the pilot study component of the Fluorescent Lyman-Alpha Structures in High-z Environments (FLASHES) Survey; the largest integral-field spectroscopy survey to date of the circumgalactic medium at z=2.3−3.1z=2.3-3.1. We observed 48 quasar fields between 2015 and 2018 with the Palomar Cosmic Web Imager (Matuszewski et al. 2010). Extended HI Lyman-α\mathrm{\alpha} emission is discovered around 42/48 of the observed quasars, ranging in projected, flux-weighted radius from 21-71 proper kiloparsecs (pkpc), with 26 nebulae exceeding 100 pkpc100\mathrm{~pkpc} in effective diameter. The circularly averaged surface brightness radial profile peaks at a maximum of 1×10−17 erg s−1 cm−2 arcsec−2\mathrm{1\times 10^{-17}~erg~s^{-1}~cm^{-2}~arcsec^{-2}} (2×10−15 erg s−1 cm−2 arcsec−22\times10^{-15}~\mathrm{erg~s^{-1}~cm^{-2}~arcsec^{-2}} adjusted for cosmological dimming) and luminosities range from 1.9×1043 erg s−11.9\times10^{43}~\mathrm{erg~s^{-1}} to −14.1×1043 erg s−1-14.1\times10^{43}~\mathrm{erg~s^{-1}}. The emission appears to have a highly eccentric morphology and a maximum covering factor of 50%50\% (60%60\% for giant nebulae). On average, the nebular spectra are red-shifted with respect to both the systemic redshift and Lyα\alpha peak of the quasar spectrum. The integrated spectra of the nebulae mostly have single or double-peaked line shapes with global dispersions ranging from 167 km s−1167~\mathrm{km~s^{-1}} to 690 km s−1690~\mathrm{km~s^{-1}}, though the individual (Gaussian) components of lines with complex shapes mostly appear to have dispersions ≤400\leq 400 km s−1\mathrm{km~s^{-1}}, and the flux-weighted velocity centroids of the lines vary by thousands of km s−1 \mathrm{km~s^{-1}} with respect to the systemic QSO redshifts. Finally, the root-mean-square velocities of the nebulae are found to be consistent with gravitational motions expected in dark matter halos of mass Mh≃1012.5M⊙\mathrm{M_h \simeq10^{12.5} M_\odot}. We compare these results to existing surveys at both higher and lower redshift
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