Planck intermediate results. XI. The gas content of dark matter halos: the Sunyaev-Zeldovich-stellar mass relation for locally brightest galaxies
Academic Article
Publication Date:
2013
abstract:
We present the scaling relation between Sunyaev-Zeldovich (SZ) signal
and stellar mass for almost 260,000 locally brightest galaxies (LBGs)
selected from the Sloan Digital Sky Survey (SDSS). These are
predominantly the central galaxies of their dark matter halos. We
calibrate the stellar-to-halo mass conversion using realistic mock
catalogues based on the Millennium Simulation. Applying a
multi-frequency matched filter to the Planck data for each LBG, and
averaging the results in bins of stellar mass, we measure the mean SZ
signal down to M* ~ 2 � 1011
M&sun;, with a clear indication of signal at even lower
stellar mass. We derive the scaling relation between SZ signal and halo
mass by assigning halo properties from our mock catalogues to the real
LBGs and simulating the Planck observation process. This relation shows
no evidence for deviation from a power law over a halo mass range
extending from rich clusters down to M500 ~ 2 �
1013 M&sun;, and there is a clear indication of
signal down to M500 ~ 4 � 1012
M&sun;. Planck's SZdetections in such low-mass halos imply
that about a quarter of all baryons have now been seen in the form of
hot halo gas, and that this gas must be less concentrated than the dark
matter in such halos in order to remain consistent with X-ray
observations. At the high-mass end, the measured SZ signal is 20% lower
than found from observations of X-ray clusters, a difference consistent
with the magnitude of Malmquist bias effects that were previously
estimated for the X-ray sample.
and stellar mass for almost 260,000 locally brightest galaxies (LBGs)
selected from the Sloan Digital Sky Survey (SDSS). These are
predominantly the central galaxies of their dark matter halos. We
calibrate the stellar-to-halo mass conversion using realistic mock
catalogues based on the Millennium Simulation. Applying a
multi-frequency matched filter to the Planck data for each LBG, and
averaging the results in bins of stellar mass, we measure the mean SZ
signal down to M* ~ 2 � 1011
M&sun;, with a clear indication of signal at even lower
stellar mass. We derive the scaling relation between SZ signal and halo
mass by assigning halo properties from our mock catalogues to the real
LBGs and simulating the Planck observation process. This relation shows
no evidence for deviation from a power law over a halo mass range
extending from rich clusters down to M500 ~ 2 �
1013 M&sun;, and there is a clear indication of
signal down to M500 ~ 4 � 1012
M&sun;. Planck's SZdetections in such low-mass halos imply
that about a quarter of all baryons have now been seen in the form of
hot halo gas, and that this gas must be less concentrated than the dark
matter in such halos in order to remain consistent with X-ray
observations. At the high-mass end, the measured SZ signal is 20% lower
than found from observations of X-ray clusters, a difference consistent
with the magnitude of Malmquist bias effects that were previously
estimated for the X-ray sample.
Iris type:
1.1 Articolo in rivista
Keywords:
cosmology: observations; cosmic background radiation; large-scale structure of Universe; galaxies: clusters: general
List of contributors:
P., Collaboration; P. A., R.; N., Aghanim; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A., Balbi; A. J., Banday; R. B., Barreiro; R., Barrena; J. G., Bartlett; E., Battaner; K., Benabed; J., Bernard; M., Bersanelli; I., Bikmaev; J. J., Bock; H., B�hringer; A., Bonaldi; J. R., Bond; J., Borrill; F. R., Bouchet; H., Bourdin; R., Burenin; C., Burigana; R. C., Butler; P., Cabella; A., Chamballu; R., Chary; L., Chiang; G., Chon; P. R., Christensen; D. L., Clements; S., Colafrancesco; S., Colombi; L. P., L.; B., Comis; A., Coulais; B. P., Crill; F., Cuttaia; A. D., Silva; H., Dahle; R. J., Davis; P. d., Bernardis; G. d., Gasperis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., D�mocl�s; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; F., Finelli; I., Flores Cacho; O., Forni; M., Frailis; E., Franceschi; M., Frommert; S., Galeotta; K., Ganga; R. T., G�nova Santos; M., Giard; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Harrison; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; G., Hurier; T. R., Jaffe; A. H., Jaffe; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; I., Khamitov; T. S., Kisner; R., Kneissl; J., Knoche; M., Kunz; H., Kurki Suonio; A., L�hteenm�ki; J., Lamarre; A., Lasenby; C. R., Lawrence; M. L., Jeune; R., Leonardi; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; G., Luzzi; J. F., Mac�as P�rez; C. J., Mactavish; B., Maffei; D., Maino; N., Mandolesi; M., Maris; F., Marleau; D. J., Marshall; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; P., Mazzotta; S., Mei; A., Melchiorri; J., Melin; L., Mendes; A., Mennella; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; H. U., N�rgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; S., Osborne; C. A., Oxborrow; F., Pajot; D., Paoletti; L., Perotto; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; R., Piffaretti; S., Plaszczynski; E., Pointecouteau; G., Polenta; L., Popa; T., Poutanen; G. W., Pratt; S., Prunet; J., Puget; J. P., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; I., Ristorcelli; G., Rocha; M., Roman; C., Rosset; M., Rossetti; Mart�n, J. A. Rubi�o.; B., Rusholme; M., Sandri; G., Savini; D., Scott; L., Spencer; J., Starck; V., Stolyarov; R., Sudiwala; R., Sunyaev; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; Terenzi, Luca; L., Toffolatti; M., Tomasi; M., Tristram; L., Valenziano; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; W., Wang; N., Welikala; J., Weller; S. D., M.; M., White; D., Yvon; A., Zacchei; A., Zonca
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