tokens: a kinematical distance of 2.0 kpc. An uncertainty of 0.5 kpc is assumed, adopting a velocity dispersion of 2.5 km s for the interstellar molecular gas. We report molecular line observations of the IRAS source using tracers of low and high density regions with the aim of studying the molecular gas content of the source, identifying dense gas clumps, finding massive young stellar objects (YSOs) linked to the clumps, and identifying possible outflows. 2. Molecular line observations IRAS 085894714 was observed with the 12 m Atacama Pathfinder EXperiment (APEX) telescope 1 , located in Llano de Chajnantor, in the Puna de Atacama, Chile. We carried out observations in the CO(32), CO(32), CO(32), HCO(32), and HCN(32) molecular lines using the On-The-Fly mapping technique. These observations were made on 2014 June 16, 19, and 21. The CO isotopes were observed with the receiver APEX2 in the spectral range of 343.8347.8 GHz and in the range 328.6332.6 GHz with a half-power beamwidth of 18, while the HCO and HCN molecules were observed with the receiver APEX1 in the spectral range of 265.6269.5 GHz with an HPBW of 22 ( Vassilev et al. 2008 ). Fig. 1 Spectra of the CO(32), CO(32), and CO(32) lines indicated in black, red, and blue, respectively. Each spectrum is the average of the profiles within a field of 25.̋5 25.̋5. The total area is 150 150 for three molecules. The locations of sources 1 (S1) and 3 (S3) are labeled. In each panel the velocity ranges from 4 to 15 km s and scales from 2 to 18 K. We mapped an area of 150 150 covering the central region of the IRAS source and the 1.2 mm emission zone detected by Beltrán et al. (2006) . The APEX1 system temperature is 150 K and 300 K for APEX2. The data reduction was performed according to the standard procedure of the CLASS software, Gildas 2 . The antenna temperature, , was transformed to main-beam brightness-temperature (), using a main beam efficiency for APEX1 and APEX2 ( Vassilev et al. 2008 ).The data were obtained with a velocity resolution of 0.11 km s. The final rms is 0.3 K. 3. Identification of YSOs To investigate the presence of YSOs coincident with the IRAS source in the Wide-field Infrared Survey Explorer (WISE) catalog ( Wright et al. 2010 ), we applied the following criteria ( Koenig et al. 2012 ). Class I objects are those that satisfy and , whereas Class II objects have and , where , , , and are the magnitudes in the four WISE bands at 3.4, 4.6, 12, and 22 m, respectively, and and are the combined errors of and , respectively 3 . Three sources with colors of Class I/II were identified. Their coordinates and correlation with 2MASS sources are indicated in Table 1 . Sources 1 and 3 are projected onto the dust clump detected by Beltrán et al. (2006) . 4. Molecular line analysis 4.1. The <inline-formula specific-use="simple-math"><sup>12</sup></inline-formula>CO, <inline-formula specific-use="simple-math"><sup>13</sup></inline-formula>CO, and C<inline-formula
ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O B-Telescope I-Telescope I-Telescope I-Telescope I-Telescope B-Telescope O O O O O B-Location I-Location I-Location O O B-Location I-Location I-Location I-Location O O O O O O B-Wavelength B-Wavelength B-Wavelength B-Wavelength O B-Wavelength O O O O B-ObservationalTechniques I-ObservationalTechniques I-ObservationalTechniques O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O B-Wavelength I-Wavelength O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O B-Instrument O O O O O B-Wavelength I-Wavelength O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O B-Wavelength B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject B-CelestialObject O B-CelestialObject B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O B-Wavelength I-Wavelength O O O O B-Citation I-Citation I-Citation I-Citation O O B-Instrument O O O O O O O O O B-Instrument O O O O O O O O O O O O B-Software I-Software B-Software I-Software O O O O O O O O O O B-TextGarbage O O O O O O B-Instrument O B-Instrument O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O B-Telescope I-Telescope I-Telescope I-Telescope B-Telescope O O B-Citation I-Citation I-Citation I-Citation O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O B-TextGarbage I-TextGarbage I-TextGarbage O O O O O O O B-Telescope O O B-Wavelength B-Wavelength B-Wavelength O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O B-Tag I-Tag B-Tag I-Tag O B-Tag