Measuring the galaxy–mass and galaxy–dust correlations through magnification and reddening

By Brice Ménard, R. Scranton, M. Fukugita, Gordon Richards. 2009

233 citations recorded by the source corpus.

We present a simultaneous detection of gravitational magnification and dust reddening effects due to galactic haloes and large-scale structure. The measurement is based on correlating the brightness of ~85 000 quasars at z > 1 with the position of 24 million galaxies at z ~ 0.3 derived from the Sloan Digital Sky Survey and is used to constrain the galaxy-mass and galaxy-dust correlation functions up to cosmological scales. The presence of dust is detected from 20 kpc to several Mpc, and we find its projected density to follow: Σ dust ~ r -0.8 p , a distribution similar to mass. On large scales, its wavelength dependence is described by R v ≃ 4.9 ± 3.2, consistent with interstellar dust. This, in turn, implies a cosmic dust density of Ω dust ≃ 5 x 10 -6 , roughly half of which comes from dust in haloes of ~L* galaxies. We estimate the resulting opacity of the Universe for various evolutionary models and find 〈A v 〉 ~ 0.03 mag up to z = 0.5. We present magnification measurements, corrected for dust extinction, from which the galaxy-mass correlation function is inferred to give the mean surface mass density profile around galaxies Σ ~ 30 (θ/1 arcmin) -0.8 h M ⊙ pc -2 up to a radius of 10 Mpc, in agreement with gravitational shear estimates.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ccd8c7b1f3a4086c8f81934b04c448a774a2a235

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Citations in the corpus

Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “The standard method extracts the magnification from correlations of distant quasars with foreground clusters, see [1059, 867].”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “…solid phase, which is remarkably close to the simulation results of Zu et al. (2011), who found that a dust mass fraction of 0.39 was required to to reproduce Ménard et al. (2010) results in a momentum-driven wind model that also reproduces observed galaxy properties and intergalactic enrichment.”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “Dust contributes significantly to the metals in the circumgalactic medium (CGM) and can be an additional cooling channel for gas (e.g. Ostriker & Silk 1973; Ménard et al. 2010; Peeples et al. 2014; Peek, Ménard & Corrales 2015).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “At shorter UV to optical wavelengths estimates of the cosmic dust abundance rely on the extinction of optical light, especially withmeasurements that combinemagnification and extinction of quasars behind samples of foreground galaxies (Ménard et al., 2010; Ménard and Fukugita, 2012).”
Observational probes of cosmic acceleration (2012, background): “Ménard et al. (2010) provide a more detailed analysis, using color information to simultaneously detect lensing magnification and reddening of quasars by dust correlated with intervening galaxies.”
THINK OUTSIDE THE COLOR BOX: PROBABILISTIC TARGET SELECTION AND THE SDSS-XDQSO QUASAR TARGETING CATALOG (2010, background): “…and their co-evolution with galaxies, e.g., through measurements of quasar clustering (e.g., Arp 1970; Hawkins & Reddish 1975; Osmer 1981; Shen et al. 2007; Ross et al. 2009), or they can be used to study the intervening intergalactic medium (e.g., Chelouche et al. 2007; Ménard et al. 2010).”
Gaseous Galaxy Halos (2012, methodology): “Ménard et al. (2010) have made a convincing detection of dust in extended galaxy 16 halos using the reddening of SDSS background quasars.”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, background): “In particular, we expect that they are invaluable in the stacked weak lensing study for which lensing signals can be detected much beyond the virial radius (e.g., Ménard et al. 2010; Umetsu et al. 2011).”
Consistent Calibration of the Tip of the Red Giant Branch in the Large Magellanic Cloud on the Hubble Space Telescope Photometric System and a Redetermination of the Hubble Constant (2019, unknown): “Impact of Blending on LMC TRGB Extinction Estimate and H0 The TRGB is commonly observed in the halos of galaxies where extinction is a scant AI ∼ 0.01 mag, as indicated by the reddening of background quasars by foreground halos at radii from the host center of 10-20 kpc (Ménard et al. 2010).”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, background): “Ménard et al. (2010) also estimate a dust density in the haloes of galaxies through a statistical measurement of reddening in background quasars when cross-correlated with SDSS galaxies.”
The Circumgalactic Medium (2017, background): “Practically, FUV lines are available at z < 1 with Hubble and z > 2 from the ground, the EUV lines can be reached at z & 0.5− 1 with Hubble (λobs & 1100 Å), and the X-ray lines can currently only be detected toward the small number of bright QSOs and blazars with reach of the sensitivity of Chandra”
THE COS-HALOS SURVEY: PHYSICAL CONDITIONS AND BARYONIC MASS IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2014, methodology): “Based on a statistical analysis of reddening using SDSS quasars behind galaxies, Ménard et al. (2010) estimate a total CGM dust mass of ∼5 × 107 M⊙.”
Cool outflows in galaxies and their implications (2020, background): “Following the pioneering work of Zaritsky (1994), studies of the reddening measurements of background quasars (Ménard et al. 2010) and passively evolving galaxies (“standard crayons”; Peek et al.”