The anomalous microwave emission (AME) has been proved to be an important component of the galactic diffuse emission in the range from 20 to 60？GHz. To discriminate between different models of AME, low frequency microwave data from 10 to 20？GHz are needed. We present here a reanalysis of published and unpublished Tenerife data from 10 to 33？GHz at large angular scales (from 5 to 15 degrees). We cross-correlate the Tenerife data to templates of the main galactic diffuse emissions: synchrotron, free-free, and thermal dust. We find evidence of dust-correlated emission in the Tenerife data that could be explained as spinning dust grain emission. 1. Introduction The anomalous microwave emission (AME) is an important contributor of the galactic diffuse emission in the range from 20 to 60？GHz. It was first identified by [1, 2] as free-free emission from electrons with temperature, ？K. Draine and Lazarian [3] argued that AME may result from electric dipole radiation due to small rotating grains, the so-called spinning dust. Models of the spinning dust emission, Draine and Lazarian [4] show that an emissivity spectrum peaking at around 20–50？GHz is able to reproduce the observations [5–12]. The initial spinning dust model has been refined regarding the shape and rotational properties of the dust grains [13–15]. An alternative explanation of AME was proposed by Draine and Lazarian [16] based on magnetic dipole radiation arising from hot ferromagnetic grains. Observations have placed limits of a few percent on the fractional polarization towards AME targets [9, 17–20]. This excludes perfectly aligned single-domain magnetic grains; however, other alignments and grain compositions produce similarly low levels of polarization [21]. A correlation between microwave and infrared maps, mainly dominated by dust thermal emission [22], was observed for various experiments, for example, on COBE/DMR [23, 24], OVRO [1, 2], Saskatoon [25, 26], survey at 19？GHz [27, 28], and Tenerife [29, 30]. A similar signal was found in compact regions by [5] and in some molecular clouds based on data from COSMOSOMAS [7, 31], AMI (Ami-Consortium: [32, 33]), CBI [9, 34], VSA [12], and Planck [35]. A recent study of the Small Magellanic Cloud also claims a detection of AME [36]. Independently, Bennett et al. [41] proposed an alternative explanation of AME based on flat-spectrum synchrotron emission associated to star-forming regions to explain part of the WMAP first-year observations. This hypothesis seems to be in disagreement with results from de Oliveira-Costa et al. [6]; Fernández-Cerezo et
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