CaltechAUTHORS
Published August 20, 2015 | Version Submitted + Published
Journal Article Open

Measurements of the Sunyaev-Zel'dovich Effect in MACS J0647.7+7015 and MACS J1206.2-0847 at High Angular Resolution with MUSTANG

Creators

  • 1. ROR icon University of Pennsylvania
  • 2. ROR icon Goddard Space Flight Center
  • 3. ROR icon United States Naval Research Laboratory
  • 4. ROR icon National Radio Astronomy Observatory
  • 5. ROR icon University of Virginia
  • 6. ROR icon California Institute of Technology
  • 7. ROR icon Trieste Astronomical Observatory
  • 8. ROR icon Institute of Astronomy and Astrophysics, Academia Sinica
  • 9. ROR icon Observatoire de la Côte d'Azur
  • 10. ROR icon Lagrange Laboratory
  • 11. ROR icon University of Trieste
  • 12. ROR icon Astronomical Observatory of Capodimonte
  • 13. ROR icon Moorpark College
  • 14. ROR icon University of Ferrara

Abstract

We present high resolution (9'') imaging of the Sunyaev–Zel'dovich Effect (SZE) toward two massive galaxy clusters, MACS J0647.7+7015 (z = 0.591) and MACS J1206.2–0847 (z = 0.439). We compare these 90 GHz measurements, taken with the Multiplexed Squid/TES Array at Ninety Gigahertz (MUSTANG ) receiver on the Green Bank Telescope, with generalized Navarro–Frenk–White (gNFW) models derived from Bolocam 140 GHz SZE data as well as maps of the thermal gas derived from Chandra X-ray observations. We adopt a serial-fitting approach, in which gNFW models are first fit to the Bolocam data and then compared to the MUSTANG data to determine an overall best-fit model. For MACS J0647.7+7015, we find a gNFW profile with core slope parameter γ = 0.9 fits the MUSTANG image with χ^2_(red) = 1.005 and probability to exceed (PTE) = 0.34. For MACS J1206.2–0847, we find γ = 0.7, χ^2_(red) = 0.993, and PTE = 0.70. In addition, we find a significant (>3σ) residual SZE feature in MACS J1206.2–0847 coincident with a group of galaxies identified in Very Large Telescope data and filamentary structure found in a weak-lensing mass reconstruction. We suggest the detected sub-structure may be the SZE decrement from a low mass foreground group or an infalling group. Giant Metrewave Radio Telescope measurements at 610 MHz reveal diffuse extended radio emission to the west, which we posit is either an active galactic nucleus-driven radio lobe, a bubble expanding away from disturbed gas associated with the SZE signal, or a bubble detached and perhaps re-accelerated by sloshing within the cluster. Using the spectroscopic redshifts available, we find evidence for a foreground (z = 0.423) or infalling group, coincident with the residual SZE feature.

Additional Information

© 2015 The American Astronomical Society. Received 2014 November 1; accepted 2015 July 20; published 2015 August 21. We thank the anonymous referee for the useful comments that helped improve this manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The GBT+MUSTANG observations presented here were obtained with telescope time allocated under NRAO proposal IDs AGBT11A009, and AGBT11B001. Additional funding was provided by NSF/AST-1309032. The Bolocam observations presented here were obtained operating from the Caltech Submillimeter Observatory, which, when the data used in this analysis were taken, was operated by the California Institute of Technology under cooperative agreement with the National Science Foundation. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. Bolocam observations were partially supported by the Gordon and Betty Moore Foundation, the Jet Propulsion Laboratory Research and Technology Development Program, as well as the National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3. The MACS J1206.2–0847 spectroscopic data were based on the ESO VLT Large Programme (prog. ID 186.A-0798, PI: P. Rosati). Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. The late night assistance of the GBT operators Greg Monk, Donna Stricklin, Barry Sharp and Dave Rose was much appreciated during the observations. Much of the work presented here was supported by NSF grant AST-0607654. Support for TM was provided by NASA through the Einstein Fellowship Program, grant PF0-110077, and through a National Research Council Research Associateship Award at the U.S. Naval Research Laboratory. Support for P.K. and A.Y. was provided by the NRAO Student Observing Support (SOS) and NASA Postdoctoral Fellowship programs. J.S. was partially supported by a Norris Foundation CCAT Postdoctoral Program Fellowship and by NSF/AST-1313447.

Attached Files

Published - Young_2015.pdf

Submitted - 1411.0317v1.pdf

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Additional details

Identifiers

Eprint ID
61320
Resolver ID
CaltechAUTHORS:20151020-102559988

Related works

Describes
http://arxiv.org/abs/1411.0317 (URL)

Funding

NSF
AST-1309032
NSF
AST-9618798
NSF
AST-0098737
NSF
AST-9980846
NSF
AST-0229008
NSF
AST-0206158
Gordon and Betty Moore Foundation
JPL Research and Technology Development Fund
National Science Council (Taipei)
NSC100-2112-M-001-008-MY3
NSF
AST-0607654
NASA Einstein Fellowship Program
PF0-110077
Naval Research Laboratory
National Radio Astronomy Observatory
NASA Postdoctoral Fellowship
Kenneth T. and Eileen L. Norris Foundation
NSF
AST-1313447
National Research Council of Canada

Dates

Created
2015-10-20
Created from EPrint's datestamp field
Updated
2021-11-10
Created from EPrint's last_modified field