Searching for radiative pumping lines of OH masers: II. The 53.3 ?m absorption line towards 1612 MHz OH maser sources*1

Abstract

This is the second paper in a series aiming at searching for infrared pumping lines for galactic 1612 MHz OH masers. Our paper I is devoted to the 34.6 µm absorption lines in ISO SWS spectra towards a large sample of galactic OH/IR sources. This paper analyzes the 53.3 µm line in the ISO LWS spectra towards a similar sample of OH/IR sources. A search with position radius of 1 arcmin in ISO Data Archive (IDA) results in 137 LWS spectra covering 53.3 µm associated with 47 galactic OH/IR sources and 4 ones associated with megamasers Arp 220 and NGC 253. (These two magamasers are included for comparison purpose only.) Ten of these galactic OH/IR sources are found to show and another 5 ones tentatively show the 53.3 µm absorption while another 7 sources (our group U1 and U2 sources) highly probably do not show this line. The source class is found to be correlated with the type of spectral profile: red supergiants (RSGs) and AGB stars tend to show strong blue-shifted filling emission in their 53.3 µm absorption line profiles while H II regions tend to show a weak red-shifted filling emission in the line profile. GC sources and megamasers mainly show symmetrical profile in the line core while megamasers tend to show an additional absorption tail on the blue side of the line profile. It is argued that the filling emission might be the manifestation of an unresolved half emission half absorption profile of the 53.3 µm doublet which might be produced by the transitions among the two levels: 2 Π 1/2 (J = 3/2) and 2 Π 1/2 (J = 5/2) and their closely related levels. The 53.3 to 34.6 µm equivalent width (EW) ratio is close to unity for RSGs but much larger than unity for GC sources and megamasers while H II regions only show the 53.3 µm line. The pump rate defined as maser to IR photon flux ratio is approximately 5% for RSGs. The pump rates of GC sources are three order of magnitude smaller. Both the large 53.3 to 34.6 µm EW ratio and the small pump rate of the GC OH masers reflect that the two detected 'pumping lines' in these sources are actually of interstellar origin. The pump rate of Arp 220 is 32%-much larger than that of RSGs, which indicates that the contribution of other pumping mechanisms to this megamaser is important. A handful of non-detections of the 34.6 or 53.3 µm line or both can be explained partly by the genuinely weakness Preprint submitted to Elsevier Science of the OH masers and partly by some other mechanisms weakening the IR pumping lines, such as clumpy OH shell or limb filling emission.⋆ Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA.

Discrete Source Survey of 6 GHz OH emission from PNe and pPNe and first 6 GHz images of K 3–35

“…From the ISO data and the non detection of these IR lines in neither of our two sources (Vy 2-2 or K 3-35, see He & Chen 2004;He et al 2005), we deduce that the line to continuum ratio is, from their 3 sigma upper limits, smaller than 0.15 and 0.19 for K 3-35 and Vy 2-2, respectively. The exact pumping efficiency is unknown but even if it would reach 25% as required by most theoretical models (see for example Elitzur et al 1976;Thai-Q-Tung et al 1998) or even by the model by Gray et al (2005) who proposed an alternative route mainly using the 53 μm photons to explain the 1612 MHz line in late type stars, we do not expect that IR pumping is playing a dominant role 7 .…”

Burst of strongly polarized maser emission at 1612 MHz in the proto-planetary nebula OH17.7–2.0

“…ISO observations of the IRC+10420 supergiant directly confirmed that the 34.6 µm photons are involved in the 1612 MHz line pumping (Sylvester et al 1997). In OH/IR and Miras the 1612 MHz maser is probably pumped by the alternative route, beginning with the 53.3 µm photons (He & Chen 2004). Therefore, if the radiative pumping is dominant in OH17.7−2.0, our observations imply that only a local rise of the infrared flux may correspond to the burst of the two 1612 MHz features.…”

Mid-Infrared Properties of Oh Megamaser Host Galaxies. Ii. Analysis and Modeling of the Maser Environment

“…There are only a few OHMs in which the important 53 μm transition has been measured (e.g., He & Chen 2004); this could be potentially observed in larger numbers of galaxies with SOFIA. The Herschel observatory can also supplement the IRS by measuring the 79 and 119 μm OH transitions in large samples of ULIRGs (e.g., Fischer et al 2010).…”