11 research outputs found
Planck intermediate results. III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and
Sunyaev-Zeldovich (SZ) effect signal D_A^2 Y for a sample of 19 objects for
which weak lensing (WL) mass measurements obtained from Subaru Telescope data
are available in the literature. Hydrostatic X-ray masses are derived from
XMM-Newton archive data and the SZ effect signal is measured from Planck
all-sky survey data. We find an M_WL-D_A^2 Y relation that is consistent in
slope and normalisation with previous determinations using weak lensing masses;
however, there is a normalisation offset with respect to previous measures
based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect
measurements are in excellent agreement with previous determinations from
Planck data. For the present sample, the hydrostatic X-ray masses at R_500 are
on average ~ 20 per cent larger than the corresponding weak lensing masses, at
odds with expectations. We show that the mass discrepancy is driven by a
difference in mass concentration as measured by the two methods, and, for the
present sample, the mass discrepancy and difference in mass concentration is
especially large for disturbed systems. The mass discrepancy is also linked to
the offset in centres used by the X-ray and weak lensing analyses, which again
is most important in disturbed systems. We outline several approaches that are
needed to help achieve convergence in cluster mass measurement with X-ray and
weak lensing observations.Comment: 19 pages, 9 figures, matches accepted versio
Planck intermediate results: III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal DA 2 Y500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an MWL-D A 2 Y500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R500 are on average ~ 20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations. © ESO, 2013.The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU).Peer Reviewe
Planck intermediate results: III. the relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal DA2 Y500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an MWL-D A2 Y500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R500 are on average ~ 20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations. © ESO, 2013
Planck intermediate results III.The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R500 are on average ~20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations
Planck intermediate results III : The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
Peer reviewe
Planck intermediate results. III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
none186We examine the relation between the galaxy cluster mass M and
Sunyaev-Zeldovich (SZ) effect signal DA2
Y500 for a sample of 19 objects for which weak lensing (WL)
mass measurements obtained from Subaru Telescope data are available in
the literature. Hydrostatic X-ray masses are derived from XMM-Newton
archive data, and the SZ effect signal is measured from Planck all-sky
survey data. We find an MWL - DA2
Y500 relation that is consistent in slope and normalisation
with previous determinations using weak lensing masses; however, there
is a normalisation offset with respect to previous measures based on
hydrostatic X-ray mass-proxy relations. We verify that our SZ effect
measurements are in excellent agreement with previous determinations
from Planck data. For the present sample, the hydrostatic X-ray masses
at R500 are on average ~ 20 percent larger than the
corresponding weak lensing masses, which is contrary to expectations. We
show that the mass discrepancy is driven by a difference in mass
concentration as measured by the two methods and, for the present
sample, that the mass discrepancy and difference in mass concentration
are especially large for disturbed systems. The mass discrepancy is also
linked to the offset in centres used by the X-ray and weak lensing
analyses, which again is most important in disturbed systems. We outline
several approaches that are needed to help achieve convergence in
cluster mass measurement with X-ray and weak lensing observations.
Appendices are available in electronic form at <A
href="http://www.aanda.org">http://www.aanda.orgP. 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;J. G. Bartlett;E. Battaner;R. Battye;K. Benabed;J. Bernard;M. Bersanelli;R. Bhatia;I. Bikmaev;H. B�hringer;A. Bonaldi;J. R. Bond;S. Borgani;J. Borrill;F. R. Bouchet;H. Bourdin;M. L. Brown;M. Bucher;R. Burenin;C. Burigana;R. C. Butler;P. Cabella;J. Cardoso;P. Carvalho;A. Chamballu;L. Chiang;G. Chon;D. L. Clements;S. Colafrancesco;A. Coulais;F. Cuttaia;A. D. Silva;H. Dahle;R. J. Davis;P. d. Bernardis;G. d. Gasperis;J. Delabrouille;J. D�mocl�s;F. D�sert;J. M. Diego;K. Dolag;H. Dole;S. Donzelli;O. Dor�;M. Douspis;X. Dupac;G. Efstathiou;T. A. En�lin;H. K. Eriksen;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;K. M. Huffenberger;G. Hurier;T. Jagemann;M. Juvela;E. Keih�nen;I. Khamitov;R. Kneissl;J. Knoche;M. Kunz;H. Kurki-Suonio;G. Lagache;J. Lamarre;A. Lasenby;C. R. Lawrence;M. L. Jeune;S. Leach;R. Leonardi;A. Liddle;P. B. Lilje;M. Linden-V�rnle;M. L�pez-Caniego;G. Luzzi;J. F. Mac�as-P�rez;D. Maino;N. Mandolesi;M. Maris;F. Marleau;D. J. Marshall;E. Mart�nez-Gonz�lez;S. Masi;S. Matarrese;F. Matthai;P. Mazzotta;P. R. Meinhold;A. Melchiorri;J. Melin;L. Mendes;S. Mitra;M. Miville-Desch�nes;L. Montier;G. Morgante;D. Munshi;P. Natoli;H. U. N�rgaard-Nielsen;F. Noviello;S. Osborne;F. Pajot;D. Paoletti;B. Partridge;T. J. Pearson;O. Perdereau;F. Perrotta;F. Piacentini;M. Piat;E. Pierpaoli;R. Piffaretti;P. Platania;E. Pointecouteau;G. Polenta;N. Ponthieu;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;C. Rosset;M. Rossetti;J. A. Rubi�o-Mart�n;B. Rusholme;M. Sandri;G. Savini;D. Scott;J. Starck;F. Stivoli;V. Stolyarov;R. Sudiwala;R. Sunyaev;D. Sutton;A. Suur-Uski;J. Sygnet;J. A. Tauber;L. Terenzi;L. Toffolatti;M. Tomasi;M. Tristram;L. Valenziano;B. V. Tent;P. Vielva;F. Villa;N. Vittorio;B. D. Wandelt;J. Weller;S. D. M.;D. Yvon;A. Zacchei;A. ZoncaP., 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; J. G., Bartlett; E., Battaner; R., Battye; K., Benabed; J., Bernard; M., Bersanelli; R., Bhatia; I., Bikmaev; H., B�hringer; A., Bonaldi; J. R., Bond; S., Borgani; J., Borrill; F. R., Bouchet; H., Bourdin; M. L., Brown; M., Bucher; R., Burenin; C., Burigana; R. C., Butler; P., Cabella; J., Cardoso; P., Carvalho; A., Chamballu; L., Chiang; G., Chon; D. L., Clements; S., Colafrancesco; A., Coulais; F., Cuttaia; A. D., Silva; H., Dahle; R. J., Davis; P. d., Bernardis; G. d., Gasperis; J., Delabrouille; J., D�mocl�s; F., D�sert; J. M., Diego; K., Dolag; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; 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; K. M., Huffenberger; G., Hurier; T., Jagemann; M., Juvela; E., Keih�nen; I., Khamitov; R., Kneissl; J., Knoche; M., Kunz; H., Kurki Suonio; G., Lagache; J., Lamarre; A., Lasenby; C. R., Lawrence; M. L., Jeune; S., Leach; R., Leonardi; A., Liddle; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; G., Luzzi; J. F., Mac�as P�rez; D., Maino; N., Mandolesi; M., Maris; F., Marleau; D. J., Marshall; E., Mart�nez Gonz�lez; S., Masi; S., Matarrese; F., Matthai; P., Mazzotta; P. R., Meinhold; A., Melchiorri; J., Melin; L., Mendes; S., Mitra; M., Miville Desch�nes; L., Montier; G., Morgante; D., Munshi; P., Natoli; H. U., N�rgaard Nielsen; F., Noviello; S., Osborne; F., Pajot; D., Paoletti; B., Partridge; T. J., Pearson; O., Perdereau; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; R., Piffaretti; P., Platania; E., Pointecouteau; G., Polenta; N., Ponthieu; 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; C., Rosset; M., Rossetti; J. A., Rubi�o Mart�n; B., Rusholme; M., Sandri; G., Savini; D., Scott; J., Starck; F., Stivoli; 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; B. D., Wandelt; J., Weller; S. D., M.; D., Yvon; A., Zacchei; A., Zonc
Planck intermediate results III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
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Planck intermediate results III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D-A(2) Y-500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M-WL-D-A(2) Y-500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R-500 are on average similar to 20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations
intermediate results
We examine the relation between the galaxy cluster mass M and
Sunyaev-Zeldovich (SZ) effect signal \hbox{\DAY} for a sample of 19 objects for which weak
lensing (WL) mass measurements obtained from Subaru Telescope data are available in the
literature. Hydrostatic X-ray masses are derived from XMM-Newton archive
data, and the SZ effect signal is measured from Planck all-sky survey
data. We find an \hbox{M_{\rm
WL}{-}\DAY} relation that is consistent in slope and
normalisation with previous determinations using weak lensing masses; however, there is a
normalisation offset with respect to previous measures based on hydrostatic X-ray
mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement
with previous determinations from Planck data. For the present sample,
the hydrostatic X-ray masses at R500 are on average
~20 percent larger than the corresponding weak lensing masses, which is contrary to
expectations. We show that the mass discrepancy is driven by a difference in mass
concentration as measured by the two methods and, for the present sample, that the mass
discrepancy and difference in mass concentration are especially large for disturbed
systems. The mass discrepancy is also linked to the offset in centres used by the X-ray
and weak lensing analyses, which again is most important in disturbed systems. We outline
several approaches that are needed to help achieve convergence in cluster mass measurement
with X-ray and weak lensing observations
Planck intermediate results. III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal
We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal DA2 Y500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an MWL - DA2 Y500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R500 are on average ~ 20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations