NIKA2 observations of dust grain evolution from star-forming filament to T-Tauri disk: Preliminary results from NIKA2 observations of the Taurus B211/B213 filament

¹ CSMES, The American University of Paris, 2bis, Passage Landrieu, 75007, Paris, France
² Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191, Gif-sur-Yvette, France
³ School of Physics and Astronomy, Cardiff University, CF24 3AA, UK
⁴ Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France
⁵ Université Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 38000 Grenoble, France
⁶ Max Planck Institute for Extraterrestrial Physics, 85748 Garching, Germany
⁷ Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
⁸ Université Grenoble Alpes, CNRS, Institut Néel, France
⁹ Institut de RadioAstronomie Millimétrique (IRAM), Grenoble, France
¹⁰ Dipartimento di Fisica, Sapienza Università di Roma, I-00185 Roma, Italy
¹¹ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
¹² Institute for Research in Fundamental Sciences (IPM), Larak Garden, 19395-5531 Tehran, Iran
¹³ Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, 28850 Madrid, Spain
¹⁴ National Observatory of Athens, IAASARS, GR-15236, Athens, Greece
¹⁵ Faculty of Physics, University of Athens, GR-15784 Zografos, Athens, Greece
¹⁶ High Energy Physics Division, Argonne National Laboratory, Lemont, IL 60439, USA
¹⁷ Instituto de Radioastronomía Milimétrica (IRAM), Granada, Spain
¹⁸ LERMA, Observatoire de Paris, PSL Research Univ., CNRS, Sorbonne Univ., UPMC, 75014 Paris, France
¹⁹ School of Earth & Space and Department of Physics, Arizona State University, AZ 85287, USA
²⁰ School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
²¹ INAF-Osservatorio Astronomico di Cagliari, 09047 Selargius, Italy
²² LPENS, ENS, PSL Research Univ., CNRS, Sorbonne Univ., Université de Paris, 75005 Paris, France
²³ Department of Physics and Astronomy, University of Pennsylvania, PA 19104, USA
²⁴ Institut d’Astrophysique de Paris, CNRS (UMR7095), 75014 Paris, France
²⁵ University of Lyon, UCB Lyon 1, CNRS/IN2P3, IP2I, 69622 Villeurbanne, France

^* e-mail: qnguyen@aup.edu

Published online: 28 March 2024

Abstract

To understand the evolution of dust properties in molecular clouds in the course of the star formation process, we constrain the changes in the dust emissivity index from star-forming filaments to prestellar and protostellar cores to T Tauri stars. Using the NIKA2 continuum camera on the IRAM 30 m telescope. we observed the Taurus B211/B2I3 filament at 1.2 mm and 2 mm with unprecedented sensitivity and used the resulting maps to derive the dust emissivity index β. Our sample of 105 objects detected in the β map of the B211/B213 filament indicates that, overal. β decreases from filament and prestellar cores (β ~ 2 ± 0.5) to protostellar cores (β ~ 1.2 ± 0.2) to T-Tauri protoplanetary disk (β < I). The averaged dust emissivity index β across the B211/B2I3 filament exhibits a flat (β ~ 2 ± 0.3) profile. This may imply that dust grain sizes are rather homogeneous in the filament, start to grow significantly in size only after the onset of the gravitational contraction/collapse of prestellar cores to protostars, reaching big sizes in T Tauri protoplanetary disks. This evolution from the parent filament to T-Tauri disks happens on a timescale of about 1-2 Myr.