NIR spectroscopy of luminous infrared galaxies and the hydrogen recombination photon deficit

¹ INAF, Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy e-mail: [valdes;bressan]@pd.astro.it
² Instituto Nacional de Astrofísica, Optica y Electrónica, Apdos. Postales 51 y 216, CP 72000 Puebla, Pue., México e-mail: jvaldes@inaoep.mx
³ Dipartimento di Astronomia, vicolo dell'Osservatorio 5, 35122 Padova, Italy e-mail: [berta;rodighiero;franceschini]@pd.astro.it
⁴ Department of Physics (Astrophysics), University of Oxford, Denys Wilkinson Building, 1 Keble Road, Oxford OX1 3RH, UK e-mail: dar@astro.ox.ac.uk

Received: 10 December 2003
Accepted: 3 January 2005

Abstract

We report on near-infrared medium-resolution spectroscopy of a sample of luminous and ultraluminous infrared galaxies (LIRGs-ULIRGs), carried out with SOFI at the ESO 3.5 m New Technology Telescope. Because of wavelength dependence of the attenuation, the detection of the Paα or Brγ line in the Ks band should provide relevant constraints on SFR and the contribution of an AGN.
We find, however, that the intensities of the Paα and Brγ lines, even corrected for slit losses, are on average only 10% and 40%, respectively, of that expected from a normal starburst of similar bolometric luminosity. The corresponding star formation rates, after correcting for the attenuation derived from the NIR-optical emission line ratios, are 14% and 60% of that expected if the far infrared luminosity were entirely powered by the starburst.
This confirms the existence of a recombination photon deficit, particularly in the case of the Paα line, already found in the Brγ line in other infrared galaxies of similar luminosity.
In discussing the possible causes of the discrepancy, we find unlikely that it is due to the presence of an AGN, though two objects show evidence of broadening of the Paα line and of the presence of coronal line emission. In fact, from our own observations and data collected from the literature we argue that the studied galaxies appear to be predominantly powered by a nuclear starburst.
Two scenarios compatible with the present data are that either there exists a highly attenuated nuclear star forming region, and/or that a significant fraction (80%) of the ionizing photons are absorbed by dust within the HII regions. We suggest that observations in the Brα spectral region could constitute a powerful tool to disentangle these two possibilities.