Ice inventory towards the protostar Ced 110 IRS4 observed with the James Webb Space Telescope

Results from the Early Release Science Ice Age program

¹ Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, NL 2300 RA Leiden, The Netherlands
² Leiden Observatory, Leiden University, PO Box 9513, NL 2300 RA Leiden, The Netherlands
³ Space Telescope Science Institute, Baltimore, MD, USA
⁴ School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
⁵ Steward Observatory, University of Arizona, Tucson, AZ, USA
⁶ Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA
⁷ Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI, USA
⁸ Institut des Sciences Moléculaires d’Orsay, CNRS, Université Paris-Saclay, Orsay, France
⁹ Centro de Astrobiología (CAB), CSIC-INTA, Ctra. de Ajalvir km 4, 28850 Torrejón de Ardoz, Spain
¹⁰ Physique des Interactions Ioniques et Moléculaires, CNRS, Aix Marseille Université, Marseille, France
¹¹ Department of Chemistry, University of California, Berkeley, Berkeley, CA, USA
¹² Max-Planck-Institut für extraterrestrische Physik, Garching bei München, Germany
¹³ Astrochemistry Laboratory, Code 691, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
¹⁴ Physical Science Department, Diablo Valley College, 321 Golf Club Road, Pleasant Hill, CA 94523, USA
¹⁵ Carl Sagan Center, SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
¹⁶ Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, USA
¹⁷ Department of Chemistry, University of British Columbia, 2036 Main Mall, Vancouver, BC, V6T 1Z1, Canada
¹⁸ Physikalisch-Meteorologisches Observatorium Davos und Weltstrahlungszentrum, Davos Dorf, Switzerland
¹⁹ Departments of Astronomy & Chemistry, University of Virginia, Charlottesville, VA, USA
²⁰ Institute of Astronomy, Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan
²¹ Center for Interstellar Catalysis, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark
²² Department of Physics, Catholic University of America, Washington, DC 20064, USA
²³ Niels Bohr Institute, University of Copenhagen, 1350 Copenhagen, Denmark
²⁴ Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Drove Drive, Pasadena, CA 91109, USA
²⁵ Department of Chemistry, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
²⁶ INAF – Osservatorio Astrofisico di Catania, Catania, Italy
²⁷ Department of Physics, University of Central Florida, Orlando, FL, USA
²⁸ Max Planck Institute for Astronomy, Heidelberg, Germany
²⁹ Southwest Research Institute, San Antonio, TX, USA

^★ Corresponding author; rocha@strw.leidenuniv.nl

Received: 15 July 2024
Accepted: 27 November 2024

Abstract

Context. Protostars contain icy ingredients necessary for the formation of potential habitable worlds, therefore, it is crucial to understand their chemical and physical environments. This work is focused on the ice features towards the binary protostellar system Ced 110 IRS4A and IRS4B, separated by 250 au and observed with James Webb Space Telescope (JWST) as part of the Early Release Science (ERS) Ice Age collaboration.

Aims. This study is aimed at exploring the JWST observations of the binary protostellar system Ced 110 IRS4A and IRS4B primarily to unveil and quantify the ice inventories towards these sources. Finally, we compare the ice abundances with those found for the same molecular cloud.

Methods. We used data from multiple JWST instruments (NIRSpec, NIRCam, and MIRI) to identify and quantify ice species in the Ced 110 IRS4 system. The analysis was performed by fitting or comparing the laboratory infrared spectra of ices to the observations. Spectral fits are carried out with the ENIIGMA fitting tool that searches for the best fit out of a large number of solutions. The degeneracies of the fits are also addressed and the ice column densities are calculated. In cases where the full nature of the absorption features is not yet known, we explore different laboratory ice spectra to compare them with the observations.

Results. We provide a list of securely and tentatively detected ice species towards the primary and the companion sources. For Ced 110 IRS4B, we detected the major ice species H₂O, CO, CO₂, and NH₃. All species are found in a mixture except for CO and CO₂, which have both mixed and pure ice components. In the case of Ced 110 IRS4A, we detected the same major species as in Ced 110 IRS4B, as well as the following minor species: CH₄, SO₂, CH₃ OH, OCN⁻, NH₄⁺, and HCOOH. A tentative detection of N₂O ice (7.75 µm), forsterite dust (11.2 µm), and CH₊⁺ gas emission (7.18 µm) in the primary source was also made. Compared with the two lines of sight towards background stars in the Chameleon I molecular cloud, the protostar exhibits similar ice abundances, except in the case of the ions that are higher in IRS4A. The most clear differences are the absence of the 7.2 and 7.4 µm absorption features due to HCOO⁻ and icy complex organic molecules in IRS4A. There is also evidence of thermal processing in both IRS4A and IRS4B, as probed by the CO₂ ice features.

Conclusions. We conclude that the binary protostellar system Ced 110 IRS4A and IRS4B has a large inventory of icy species. The similar ice abundances in comparison to the starless regions in the same molecular cloud suggests that the chemical conditions of the protostar were set at earlier stages in the molecular cloud. It is also possible that the source inclination and complex geometry cause a low column density along the line of sight, which hides the bands at 7.2 and 7.4 µm. Finally, we highlight that a comprehensive analysis using radiative transfer modelling is needed to disentangle the spectral energy distributions of these sources.