TY - JOUR
T1 - Star formation in IC1396
T2 - Kinematics and subcluster structure revealed by Gaia
AU - Pelayo-Baldárrago, Mara E.
AU - Sicilia-Aguilar, Aurora
AU - Fang, Min
AU - Roccatagliata, Veronica
AU - Kim, Jinyoung Serena
AU - García-Álvarez, David
N1 - Funding Information:
We thank the anonymous referee for providing valuable comments that helped to clarify this paper. M.P.B. is supported by the funding of the Peruvian National Council of Science, Technology and Technological Innovation (“Consejo Nacional de Ciencia, Tecnología e Innovación Tecnológica-CONCYTEC)”) via a predoctoral grant, contract “033-2016-FONDECYT (Peru)”. We thank Konstantin Getman for his valuable comments and for providing his unpublished list of X-ray sources for complete the collection of known members. Observations reported here include data obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution, and observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work is (partly) based on data obtained with the instrument OSIRIS, built by a Consortium led by the Instituto de Astrofísica de Canarias in collaboration with the Instituto de Astronomía of the Universidad Autónoma de México. OSIRIS was funded by GRANTECAN and the National Plan of Astronomy and Astrophysics of the Spanish Government. This work is based on observations collected at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). This work has made use of data from: the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement; from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation, and from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We also have made use of data products of the SIMBAD database, of the VizieR catalog access tool, operated at CDS, Strasbourg, France, and of Astropy ( http://www.astropy.org ), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018).
Publisher Copyright:
© 2023 EDP Sciences. All rights reserved.
PY - 2023/1/1
Y1 - 2023/1/1
N2 - Aims. We investigate the star formation history of the IC1396 region by studying its kinematics and completing the population census. Methods. We used multiwavelength data, combining optical spectroscopy to identify and classify new members and near-infrared photometry to trace shocks, jets, and outflows as well as the interactions between the cluster members and the cloud. We also used Gaia EDR3 data to identify new potential members in the multidimensional proper motion and parallax space. Results. The revised Gaia EDR3 distance is 925±73 pc, slightly closer than previously obtained with DR2. The Gaia data reveal four distinct subclusters in the region. These subclusters are consistent in distance but display differences in proper motion. This result, with their age differences, hints toward a complex and varied star formation history. The Gaia data also unveil intermediate-mass objects that tend to evade spectroscopic and disk surveys. Our analysis has allowed us to identify 334 new members. We estimate an average age of ~4 Myr, confirming previous age estimates. With the new members added to our study, we estimate a disk fraction of 28%, lower than previous values, due to our method detecting mainly new, diskless, intermediate-mass stars. We find age differences between the subclusters, which offers evidence of a complex star formation history with different episodes of star formation.
AB - Aims. We investigate the star formation history of the IC1396 region by studying its kinematics and completing the population census. Methods. We used multiwavelength data, combining optical spectroscopy to identify and classify new members and near-infrared photometry to trace shocks, jets, and outflows as well as the interactions between the cluster members and the cloud. We also used Gaia EDR3 data to identify new potential members in the multidimensional proper motion and parallax space. Results. The revised Gaia EDR3 distance is 925±73 pc, slightly closer than previously obtained with DR2. The Gaia data reveal four distinct subclusters in the region. These subclusters are consistent in distance but display differences in proper motion. This result, with their age differences, hints toward a complex and varied star formation history. The Gaia data also unveil intermediate-mass objects that tend to evade spectroscopic and disk surveys. Our analysis has allowed us to identify 334 new members. We estimate an average age of ~4 Myr, confirming previous age estimates. With the new members added to our study, we estimate a disk fraction of 28%, lower than previous values, due to our method detecting mainly new, diskless, intermediate-mass stars. We find age differences between the subclusters, which offers evidence of a complex star formation history with different episodes of star formation.
KW - Globular clusters: individual: IC1396
KW - H II regions
KW - ISM: jets and outflows
KW - Stars: formation
KW - Stars: pre-main sequence
KW - Techniques: spectroscopic
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U2 - 10.1051/0004-6361/202244265
DO - 10.1051/0004-6361/202244265
M3 - Article
AN - SCOPUS:85145431627
SN - 0004-6361
VL - 669
JO - Astronomy and astrophysics
JF - Astronomy and astrophysics
M1 - A22
ER -