THE SERENDIPITOUS OBSERVATION OF A GRAVITATIONALLY LENSED GALAXY AT z=0.9057 FROM THE BLANCO COSMOLOGY SURVEY: THE ELLIOT ARC

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題名:	THE SERENDIPITOUS OBSERVATION OF A GRAVITATIONALLY LENSED GALAXY AT z=0.9057 FROM THE BLANCO COSMOLOGY SURVEY: THE ELLIOT ARC
作者:	Buckley-Geer,EJ;Lin,H;Drabek,ER;Allam,SS;Tucker,DL;Armstrong,R;Barkhouse,WA;Bertin,E;Brodwin,M;Desai,S;Frieman,JA;Hansen,SM;High,FW;Mohr,JJ;Lin,YT;Ngeow,CC;Rest,A;Smith,RC;Song,J;Zenteno,A
貢獻者:	天文研究所
關鍵詞:	DIGITAL SKY SURVEY;XMM-NEWTON OBSERVATION;DARK-MATTER;STAR-FORMATION;RICHNESS RELATION;LEGACY SURVEY;CLUSTER;WEAK;MASS;MAXBCG
日期:	2011
上傳時間:	2012-03-27 18:13:05 (UTC+8)
出版者:	國立中央大學
摘要:	We report on the serendipitous discovery in the Blanco Cosmology Survey (BCS) imaging data of a z = 0.9057 galaxy that is being strongly lensed by a massive galaxy cluster at a redshift of z = 0.3838. The lens (BCS J2352-5452) was discovered while examining i- and z-band images being acquired in 2006 October during a BCS observing run. Follow-up spectroscopic observations with the Gemini Multi-Object Spectrograph instrument on the Gemini-South 8 m telescope confirmed the lensing nature of this system. Using weak-plus-strong lensing, velocity dispersion, cluster richness N(200), and fitting to a Navarro-Frenk-White (NFW) cluster mass density profile, we have made three independent estimates of the mass M(200) which are all very consistent with each other. The combination of the results from the three methods gives M(200) = (5.1 +/- 1.3) x 10(14) M(circle dot), which is fully consistent with the individual measurements. The final NFW concentration c(200) from the combined fit is c(200) = 5.4(1.1)(+1.4) We have compared our measurements of M(200) and c(200) with predictions for (1) clusters from ACDM simulations, (2) lensing-selected clusters from simulations, and (3) a real sample of cluster lenses. We find that we are most compatible with the predictions for ACDM simulations for lensing clusters, and we see no evidence based on this one system for an increased concentration compared to ACDM. Finally, using the flux measured from the [O(II)]3727 line we have determined the star formation rate of the source galaxy and find it to be rather modest given the assumed lens magnification.
關聯:	ASTROPHYSICAL JOURNAL
顯示於類別:	[天文研究所] 期刊論文

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