Chemical modeling of the L1498 and L1517B prestellar cores: CO and HCO⁺ depletion^⋆,⋆⋆

¹ UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), UMR 5274, 38041 Grenoble, France
e-mail: sebastien.maret@obs.ujf-grenoble.fr
² Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48104, USA
³ Observatorio Astronómico Nacional, Alfonso XII 3, 28014 Madrid, Spain

Received: 14 June 2013
Accepted: 18 September 2013

Abstract

Prestellar cores exhibit a strong chemical differentiation, which is mainly caused by the freeze-out of molecules onto the grain surfaces. Understanding this chemical structure is important, because molecular lines are often used as probes to constrain the core physical properties. Here we present new observations and analysis of the C¹⁸O (1–0) and H¹³CO⁺ (1–0) line emission in the L1498 and L1517B prestellar cores, located in the Taurus-Auriga molecular complex. We model these observations with a detailed chemistry network coupled to a radiative transfer code. Our model successfully reproduces the observed C¹⁸O (1–0) emission for a chemical age of a few 10⁵ years. On the other hand, the observed H¹³CO⁺ (1–0) is reproduced only if cosmic-ray desorption by secondary photons is included, and if the grains have grown to a bigger size than average ISM grains in the core interior. This grain growth is consistent with the infrared scattered light (“coreshine”) detected in these two objects, and is found to increase the CO abundance in the core interior by about a factor four. According to our model, CO is depleted by about 2–3 orders of magnitude in the core center.