Evolution in the X‐Ray Cluster Luminosity Function Revisited

Nichol, R. C.; Holden, B. P.; Romer, A. K.; Ulmer, M. P.; Burke, Douglas; Collins, Chris

doi:10.1086/304061

Cited by 55 publications

(88 citation statements)

References 30 publications

(45 reference statements)

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“…Finally, the XCLF presented here is fully consistent with other measurements and adds new information regarding the existence of a "deficit" of high redshift, high luminosity clusters which has been debated by many authors (e.g. Reichart et al 1999;Nichol et al 1999;Gioia et al 1999). This is because the SRC covers a large area of sky (≃ 300deg 2 at present) which is vital for detecting massive, X-ray bright clusters at high redshift (see Ebeling et al 2000).…”

Section: The Sdss-rass Cluster Catalogsupporting

confidence: 87%

SDSS-RASS: Next Generation of Cluster-Finding Algorithms

Nichol¹,

Miller²,

Connolly³

et al. 2003

Eso Astrophysics Symposia

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Section: The Sdss-rass Cluster Catalogsupporting

confidence: 87%

SDSS-RASS: Next Generation of Cluster-Finding Algorithms

Nichol¹,

Miller²,

Connolly³

et al. 2003

Eso Astrophysics Symposia

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“…In R00, the Nichol et al (1997) empirical Ðt to the o †-axis PSF degradation was used. The Nichol et al (1997) PSF was symmetric whereas, in reality, the PSF is not symmetric.…”

Section: Details Of the Simulation Processmentioning

confidence: 99%

“…In R00, the Nichol et al (1997) empirical Ðt to the o †-axis PSF degradation was used. The Nichol et al (1997) PSF was symmetric whereas, in reality, the PSF is not symmetric. The asymmetry was important to take into account in our In Table 1 we summarize the parameters used during each of the 20 di †erent simulation runs.…”

Section: Details Of the Simulation Processmentioning

confidence: 99%

The Bright SHARC Survey: The Selection Function and Its Impact on the Cluster X‐Ray Luminosity Function

Adami¹,

Ulmer

Romer

et al. 2000

ASTROPHYS J SUPPL S

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We present the results of a comprehensive set of simulations designed to quantify the selection function of the Bright SHARC survey for distant clusters. The statistical signiÐcance of the simulations relied on the creation of many thousands of artiÐcial clusters with redshifts and luminosities in the range 0.25 \ z \ 0.95 and ergs s~1 (0.5È2.0 keV). We created one standard and 19 varied 0.5 \ L X \ 10 ] 1044 distribution functions, each of which assumed a di †erent set of cluster, cosmological and operational parameters. The parameters we varied included the values of b, core radius and ellipticityWe also investigated how nonstandard surface brightness proÐles (i.e., the Navarro, Frenk, & White, or NFW, model) ; cooling Ñows ; and the ROSAT pointing target, inÑuence the selection function in the Bright SHARC survey. For our standard set we adopted the parameters used during the derivation of the Bright SHARC Cluster X-Ray Luminosity Function (CXLF), i.e., and an isothermal ) 0 \ 1, ) " \ 0 b model with b \ 0.67, kpc, and e \ 0.15. We found that certain parameters have a dramatic r c \ 250 e †ect on our ability to detect clusters, e.g., the presence of a NFW proÐle or a strong cooling Ñow proÐle, or the value of and b. Other parameters had very little e †ect, e.g., the type of ROSAT target r c and the cluster ellipticity. At distant redshift (z [ 0.8), elliptical clusters are signiÐcantly easier to detect than spherical ones in the Bright SHARC survey. We show also that all the tested parameters have only a small inÑuence on the computed luminosity of the clusters ("" recovered luminosity ÏÏ in the text) except the presence of a strong cooling Ñow. We conclude that the CXLF presented by Nichol et al. in 1999 is robust (under the assumption of standard parameters), but stress the importance of cluster follow-up, by Chandra and XMM, in order to better constrain the morphology of the distant clusters found in the Bright SHARC and other surveys.

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“…case of the EMSS, this quantity is given by (Avni & Bahcall 1980 ;Henry et al 1992 ;Nichol et al 1997)…”

Section: T He X-ray Cluster L Uminosity Functionmentioning

confidence: 99%

“…The original EMSS consists of 93 X-ray clusters, of which 67 have redshifts z º 0.14. Nichol et al (1997) updated this z º 0.14 subsample with 21 ROSAT luminosities and optical information from the literature. This revised EMSS consists of 64 X-ray clusters, of which 25 have been updated.…”

Section: Introductionmentioning

confidence: 99%

Untitled

1999

ApJ

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From the Press-Schechter mass function and the empirical X-ray cluster luminosity-temperature (L -T ) relation, we construct an X-ray cluster luminosity function that can be applied to the growing number of high-redshift, X-ray cluster luminosity catalogs to constrain cosmological parameters. In this paper, we apply this luminosity function to the Einstein Medium Sensitivity Survey (EMSS) and the ROSAT Brightest Cluster Sample (BCS) luminosity function to constrain the value ofIn the case of the ) m . EMSS, we Ðnd a factor of 4È5 fewer X-ray clusters at redshifts above z \ 0.4 than below this redshift at luminosities above ergs s~1 (0.3È3.5 keV), which suggests that the X-ray cluster lumi-L X\ 7 ] 1044 nosity function has evolved above At lower luminosities, this luminosity function evolves only mini-L | . mally, if at all. Using Bayesian inference, we Ðnd that the degree of evolution at high luminosities suggests that given the best-Ðt L -T relation of Reichart, Castander, & Nichol. When we ) m \ 0.96~0 .32 0.36, account for the uncertainty in how the empirical L -T relation evolves with redshift, we Ðnd that ) m B 1.0^0.4. However, it is unclear to what degree systematic e †ects may a †ect this and similarly obtained results.

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Evolution in the X‐Ray Cluster Luminosity Function Revisited

Cited by 55 publications

References 30 publications

SDSS-RASS: Next Generation of Cluster-Finding Algorithms

SDSS-RASS: Next Generation of Cluster-Finding Algorithms

The Bright SHARC Survey: The Selection Function and Its Impact on the Cluster X‐Ray Luminosity Function

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