SIMBAD references

2007AJ....134.2366I - Astron. J., 134, 2366-2384 (2007/December-0)

Millimeter interferometric HCN(1-0) and HCO+(1-0) observations of luminous infrared galaxies.


Abstract (from CDS):

We present the results on millimeter interferometric observations of four luminous infrared galaxies (LIRGs), Arp 220, Mrk 231, IRAS 08572+3915, and VV 114, and one Wolf-Rayet galaxy, He 2-10, using the Nobeyama Millimeter Array (NMA). Both the HCN(1-0) and HCO+(1-0) molecular lines were observed simultaneously, and their brightness-temperature ratios were derived. High-quality infrared L-band (2.8-4.1 µm) spectra were also obtained for the four LIRGs to better constrain their energy sources deeply buried in dust and molecular gas. When combined with other LIRGs we have previously observed with NMA, the final sample comprised nine LIRGs (12 LIRG nuclei) with available interferometric HCN(1-0) and HCO+(1-0) data, sufficient to investigate the overall trend in comparison with known AGNs and starburst galaxies. We found that LIRGs with luminous buried AGN signatures at other wavelengths tend to show high HCN(1-0)/HCO+(1-0) brightness-temperature ratios as seen in AGN-dominated galaxies, while the Wolf-Rayet galaxy He 2-10 displays a small ratio. An enhanced HCN abundance in the interstellar gas surrounding a strongly X-ray-emitting AGN, as predicted by some chemical calculations, and/or infrared radiative pumping, are possible explanations of our results.

Abstract Copyright:

Journal keyword(s): Galaxies: Active - Galaxies: Individual: Name: Arp 220 - Galaxies: Individual: Name: Markarian 231 - Galaxies: Individual: Alphanumeric: IRAS 08572+3915 - Galaxies: Individual: Alphanumeric: VV 114 - galaxies: individual (He 2-10) - Galaxies: ISM - Galaxies: Nuclei - Radio Lines: Galaxies

Simbad objects: 28

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2007AJ....134.2366I and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact