Deep spectroscopic observations of a z=4.3 HyLIRG with indications of Pa alpha and PAH emission

Details Deep spectroscopic observations of a z=4.3 HyLIRG with indications of Pa alpha and PAH emission Deep spectroscopic observations of a z=4.3 HyLIRG with indications of Pa alpha and PAH emission

Aug 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop..494d&link_type=abstract

Spitzer Proposal ID #494

Physics

Scientific paper

We request IRS observations of J1717+6009, a z=4.27 source that is an outlier in redshift, IR luminosity, and spectral properties in the 5mJy Spectroscopic Legacy project 5MUSES, which surveyed the XFLS, ELAIS-N1, ELAIS-N2, XMM, and Lockman Hole fields. With rest-frame 4.6 and 13.3 micron luminosities of 5*10^13 L_sun, this source is a bright Hyperluminous Infrared Galaxy. Its rest-frame UV/optical spectra show broad absorption lines that are associated with strong outflows. J1717+6009 is an exceptionally rare candidate for the study of coeval AGN accretion, feedback, and star-formation activity at z>4. It is unique because it shows tentative evidence for both hydrogen recombination and PAH feature emission in the MIR. The existing ~4-min long IRS observations per spectral order, which were obtained after the cycle 5 deadline, have low S/N (4.5-7.5 sigma) detections at the Pa alpha, the PAH 3.3, and the PAH 6.2 micron wavelengths. We request new IRS observations, which will last in total 5.1 hours, to allow for a reliable detection of the 3.3 and 6.2 micron PAH features and several rest-frame NIR hydrogen lines. The flux ratios of NIR and optical/UV hydrogen lines will help us estimate the AGN gas column density. The widths of the broad hydrogen lines can constrain the mass and the accretion rate of the black hole in this AGN. The luminosity of the PAH features will help us estimate the star formation that the host galaxy is undergoing. If successful, these deep observations will establish Spitzer as the observatory to pioneer the detection of PAHs at z>4, and will lay the foundations for the use of the JWST MIRI instrument for the study of star formation up to the era of reionization using the 3.3 micron PAH feature.

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