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Published April 1, 2016 | Published + Submitted
Journal Article Open

Peculiar Velocity Constraints from Five-Band SZ Effect Measurements Towards RX J1347.5-1145 with MUSIC and Bolocam from the CSO


We present Sunyaev-Zel'dovich (SZ) effect measurements from wide-field images towards the galaxy cluster RX J1347.5-1145 obtained from the Caltech Submillimeter Observatory with the Multiwavelength Submillimeter Inductance Camera (MUSIC) at 147, 213, 281, and 337 GHz and with Bolocam at 140 GHz. As part of our analysis, we have used higher frequency data from Herschel-SPIRE and previously published lower frequency radio data to subtract the signal from the brightest dusty star-forming galaxies behind RX J1347.5-1145 and from the AGN in RX J1347.5-1145's BCG. Using these five-band SZ effect images, combined with previously published X-ray spectroscopic measurements of the temperature of the intra-cluster medium (ICM) from Chandra, we constrain the ICM optical depth to be τ_e = 2.73^(+0.38)_(-0.39) x 10^(-3) and the ICM line of sight peculiar velocity to be v_(pec) = -1260^(+760)_(-530) km s^(-1). The errors for both quantities are limited by measurement noise rather than calibration uncertainties or astrophysical contamination, and significant improvements are possible with deeper observations. Our best-fit velocity is in mild tension with the two previously published SZ effect measurements for RX J1347.5-1145, although some or all of the tension may be because those measurements sample the cluster differently.

Additional Information

© 2016 The American Astronomical Society. Received 2015 September 9; accepted 2016 February 20; published 2016 March 24. We thank the anonymous referee for his or her extensive suggestions to improve this manuscript. We acknowledge the assistance of: the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during data-taking for this data set; Kathy Deniston and Diana Bisel, who provided effective administrative support at Caltech and in Hilo; J.S. was partially supported by a Norris Foundation Fellowship; N.G.C. was partially supported by a NASA Graduate Student Research Fellowship; S.R.S. was supported by a NASA Earth and Space Science Fellowship; MUSIC was constructed and commissioned with funding provided by the Gordon and Betty Moore Foundation, JPL internal funds, and the NSF Advanced Technologies and Instrumentation (ATI) and Astronomy and Astrophysics Grants (AAG) Programs. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with a significant participation by NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. This research was performed while TM held a National Research Council Research Associateship Award at the Naval Research Laboratory. Facilities: CSO - , Chandra - , Herschel - European Space Agency's Herschel space observatory.

Attached Files

Published - apj_820_2_101.pdf

Submitted - 1509.02950v1.pdf


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