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The interstellar medium is crucial to understanding the physics of activegalaxies and the coevolution between supermassive black holes and their hostgalaxies. However, direct gas measurements are limited by sensitivity and otheruncertainties. Dust provides an efficient indirect probe of the total gas. Weapply this technique to a large sample of quasars, whose total gas contentwould be prohibitively expensive to measure. We present a comprehensive studyof the full (1 to 500 micron) infrared spectral energy distributions of 87redshift <0.5 quasars selected from the Palomar-Green sample, using photometricmeasurements from 2MASS, WISE, and Herschel, combined with Spitzer mid-infrared(5 to 40 micron) spectra. With a newly developed Bayesian Markov Chain MonteCarlo fitting method, we decompose various overlapping contributions to theintegrated spectral energy distribution, including starlight, warm dust fromthe torus, and cooler dust on galaxy scales. This procedure yields a robustdust mass, which we use to infer the gas mass, using a gas-to-dust ratioconstrained by the host galaxy stellar mass. Most (90%) quasar hosts have gasfractions similar to those of massive, star-forming galaxies, although aminority (10%) seem genuinely gas-deficient, resembling present-day massiveearly-type galaxies. This result indicates that "quasar mode" feedback does notoccur or is ineffective in the host galaxies of low-redshift quasars. We alsofind that quasars can boost the interstellar radiation field and heat dust ongalactic scales. This cautions against the common practice of using thefar-infrared luminosity to estimate the host galaxy star formation rate.

On the Gas Content and Efficiency of AGN Feedback in Low-redshift Quasars