Galaxy Cluster Gas Mass Fractions from Sunyaev-Zeldovich Effect Measurements: Constraints on ΩM

By L. Grego, J. Carlstrom, E. Reese, G. Holder, W. Holzapfel, M. Joy, Joseph J. Mohr, S. Patel. 2000

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Using sensitive centimeter-wave receivers mounted on the Owens Valley Radio Observatory and Berkeley-Illinois-Maryland-Association millimeter arrays, we have obtained interferometric measurements of the Sunyaev-Zeldovich (SZ) effect toward massive galaxy clusters. We use the SZ data to determine the pressure distribution of the cluster gas and, in combination with published X-ray temperatures, to infer the gas mass and total gravitational mass of 18 clusters. The gas mass fraction, fg, is calculated for each cluster and is extrapolated to the fiducial radius r500 using the results of numerical simulations. The mean fg within r500 is 0.081 h (statistical uncertainty at 68% confidence level, assuming ΩM = 0.3, ΩΛ = 0.7). We discuss possible sources of systematic errors in the mean fg measurement. We derive an upper limit for ΩM from this sample under the assumption that the mass composition of clusters within r500 reflects the universal mass composition: ΩMh ≤ ΩB/fg. The gas mass fractions depend on cosmology through the angular diameter distance and the r500 correction factors. For a flat universe (ΩΛ ≡ 1 - ΩM) and h = 0.7, we find the measured gas mass fractions are consistent with ΩM < 0.40, at 68% confidence. Including estimates of the baryons contained in galaxies and the baryons which failed to become bound during the cluster formation process, we find ΩM ~ 0.25.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9101bc787409319a63d2ef5955cdf573f600e28e

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In Astronomy and Astrophysics

1. S. Allen
2. H. Ebeling
3. David Rapetti
4. Andrey V. Kravtsov
5. R. Schmidt
6. J. Carlstrom
7. Joseph J. Mohr
8. M. Joy

Citations in the corpus

• Determining the Cosmic Distance Scale from Interferometric Measurements of the Sunyaev-Zeldovich Effect (2002, methodology): “…are now routinely producing high quality images of the SZE (Jones et al. 1993; Grainge et al. 1993; Carlstrom et al. 1996; Carlstrom et al. 1998; Saunders et al. 1999; Grainge et al. 2002b; Reese et al. 2000; Grego et al. 2000; Carlstrom et al. 2000; Grego et al. 2001; Jones et al. 2002).”
• X-Ray and Sunyaev-Zel’dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters (2006, methodology): “(14) Under the isothermal assumption, this reduces to the simple analytic form (e.g., Grego et al. 2001): Mtotal(r) = 3βkTe Gµmp r3 r2c + r 2 , (15) which can be used to calculate total masses for both the 100 kpc-cut and SZE-only models.”
• Determination of the Cosmic Distance Scale from Sunyaev-Zel’dovich Effect and Chandra X-Ray Measurements of High-Redshift Galaxy Clusters (2005, background): “…et al. 1999), while interferometric observations at centimeter wavelengths have produced images of the SZE (Jones et al. 1993; Grainge et al. 1993; Carlstrom et al. 1996, 2000; Grainge et al. 2002; Reese et al. 2000, 2002; Grego et al. 2000, 2001; La Roque et al. 2003; Udomprasert et al. 2004).”
• The Search for the Missing Baryons at Low Redshift (2007, background): “This effect is seen toward rich clusters of galaxies through dedicated observations (Grego et al., 2001), and even in the survey data from the first year of Wilkinson Microwave Anisotrpy Probe (WMAP), it is detected (Hernández-Monteagudo et al., 2004).”
• Quasar Feedback: The Missing Link in Structure Formation (2004, unknown): “This so-called Sunyaev-Zel’dovich effect (Sunyaev & Zel’dovich 1972) has been well studied theoretically (e.g., Aghanim et al. 1997; Refregier et al. 2000) and detected in a number of clusters (e.g., Grego et al. 2001; Reese et al. 2002).”
• Near-Infrared Properties of Galaxy Clusters: Luminosity as a Binding Mass Predictor and the State of Cluster Baryons (2003, methodology): “Grego et al. (2001) estimated ΩM ∼ 0.25 from the SZE observations of 18 clusters.”
• Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, background): “…David, Jones & Forman 1995; White & Fabian 1995; Evrard 1997; Mohr, Mathiesen & Evrard 1999; Ettori & Fabian 1999; Roussel, Sadat & Blanchard 2000; Grego et al. 2001; Allen, Schmidt & Fabian 2002a; Allen et al. 2003, 2004; Ettori, Tozzi & Rosati 2003; Sanderson & Ponman 2003; Lin, Mohr &…”