Erratum: ``The Fundamental Plane for z = 0.8-0.9 Cluster Galaxies'' ( ApJ 639, L9 [2006])

Details Erratum: ``The Fundamental Plane for z = 0.8-0.9 Cluster Galaxies'' ( ApJ 639, L9 [2006]) Erratum: ``The Fundamental Plane for z = 0.8-0.9 Cluster Galaxies'' ( ApJ 639, L9 [2006])

Jan 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...654l.179j&link_type=abstract

The Astrophysical Journal, Volume 654, Issue 2, pp. L179-L180.

Astronomy and Astrophysics

Astrophysics

11

Scientific paper

In the above-mentioned Letter, an incorrect calibration of the photometry to the rest-frame B band was used for the two high-redshift clusters RX J0152.7-1357 (z=0.83) and RX J1226.9+3332 (z=0.89). This error was identified with the help of P. van Dokkum. To correct for the error, the photometry for the two high-redshift clusters should be offset to brighter luminosities with a factor (1+zcluster), corresponding to an average offset in logL for the two clusters of log(1+0.86)=0.27.
With this error corrected, the fundamental plane (FP) for the two high-redshift clusters (eq. [2] in the above-mentioned Letter) should readlogre=(0.60+/-0.22)logσ-(0.70+/-0.06)loge+1.32. (1)The relation between the galaxy masses and the mass-to-light ratio (eq. [4] in the above-mentioned Letter) should readlog(M/L)=(0.54+/-0.08)logM-5.74. (2)We include a revised version of Figure 1 that reflects these changes.
The discussion of the possible systematic effects and the simulations supporting the conclusion that the FP is steeper for the high-redshift sample compared to that of the Coma Cluster remain unchanged (§ 4 and Fig. 2 of the above-mentioned Letter).
The offsets and relations stated in § 5 in the above-mentioned Letter change as follows. The median offset of log(M/L) for the high-redshift sample relative to the Coma sample is -0.65, corresponding to an epoch of the last major star formation episode of zform~1.3. The mass-dependent difference in log(M/L) between the high- and low-redshift samples is Δlog(M/L)=-0.30logM+3.99, equivalent to Δlog(age)=-0.32logM+4.27. Thus, for the lowest mass galaxies (1010.3 Msolar), the last epoch of star formation may have been as recent as zform~1.1. This is only ~1 Gyr prior to when the light that we now observe was emitted from the galaxies in the high-redshift sample. For galaxies with M~1010.8 Msolar, we find zform~1.25, while for galaxies with M>1011.3 Msolar, we find zform>~1.6.
As the revised Figure 1 shows, the predictions from Thomas et al. (2005) are in quite good agreement with our high-redshift data, and no offset to higher look-back times is needed.
The remainder of the above-mentioned Letter is unaffected by the error in the calibration. The authors regret the mistake and thank P. van Dokkum for assisting in identifying this problem.