CaltechAUTHORS
Published September 20, 2009 | Version Published
Journal Article Open

A Bright Submillimeter Source in the Bullet Cluster (1E0657-56) Field Detected with Blast

Creators

  • 1. ROR icon University of Pennsylvania
  • 2. ROR icon Cardiff University
  • 3. ROR icon National Institute of Astrophysics, Optics and Electronics
  • 4. ROR icon Jet Propulsion Lab
  • 5. ROR icon California Institute of Technology
  • 6. ROR icon University of British Columbia
  • 7. ROR icon University of Miami
  • 8. ROR icon Canadian Institute for Theoretical Astrophysics
  • 9. ROR icon University of Toronto
  • 10. ROR icon University of Puerto Rico System
  • 11. ROR icon Astroparticle and Cosmology Laboratory
  • 12. ROR icon Brown University

Abstract

We present the 250, 350, and 500 μm detection of bright submillimeter emission in the direction of the Bullet Cluster measured by the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). The 500 μm centroid is coincident with an AzTEC 1.1 mm point-source detection at a position close to the peak lensing magnification produced by the cluster. However, the 250 μm and 350 μm centroids are elongated and shifted toward the south with a differential shift between bands that cannot be explained by pointing uncertainties. We therefore conclude that the BLAST detection is likely contaminated by emission from foreground galaxies associated with the Bullet Cluster. The submillimeter redshift estimate based on 250-1100 μm photometry at the position of the AzTEC source is z_(phot) = 2.9^(+0.6)_(–0.3), consistent with the infrared color redshift estimation of the most likely Infrared Array Camera counterpart. These flux densities indicate an apparent far-infrared (FIR) luminosity of L_(FIR) = 2 × 10^(13) L_☉ . When the amplification due to the gravitational lensing of the cluster is removed, the intrinsic FIR luminosity of the source is found to be L_(FIR) ≤ 10^(12) L_☉, consistent with typical luminous infrared galaxies.

Additional Information

© 2009 American Astronomical Society. Print publication: Issue 1 (2009 September 20); received 2009 April 7; accepted for publication 2009 July 29; published 2009 August 27. We acknowledge the support of NASA through grant NAG5- 12785, NAG5- 13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). We thank Tony Mroczkowski for his help with the SZE simulations. This research has been enabled by the use of West- Grid computing resources. This research also made use of the SIMBAD database, observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and SAOImage DS9, developed by Smithsonian Astrophysical Observatory.

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Additional details

Identifiers

Eprint ID
16074
Resolver ID
CaltechAUTHORS:20090928-115957244

Funding

NASA
NAG5-12785
NASA
NAG5-13301
NASA
NNGO-6GI11G
NSF
Canadian Space Agency (CSA)
Natural Sciences and Engineering Research Council of Canada (NSERC)
Science and Technology Facilities Council (STFC)

Dates

Created
2009-09-28
Created from EPrint's datestamp field
Updated
2021-11-08
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Caltech groups
Physics Department