SCYON Abstract

Received on April 18 2012

Multiwavelength Study of NGC 281 Region

AuthorsSaurabh Sharma (1,2,3), A.K. Pandey (1), J.C. Pandey (1), N. Chauhan (1,8), K. Ogura (4), D.K. Ojha (5), J. Borrissova (2), H. Mito (6), T. Verdugo (2,9), and B.C. Bhatt (7)
Affiliation(1) Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263 129, India
(2) Departamento de Fíisica y Astronomía, Universidad de Valparaíso, Ave. Gran Bretana 1111, Valparaíso, Chile
(3) INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
(4) Kokugakuin University, Higashi, Shibuya-ku, Tokyo 150-8440, Japan
(5) Tata Institute of Fundamental Research, Mumbai - 400 005, India
(6) Kiso Observatory, School of Science, University of Tokyo, Mitake-mura, Kiso-gun, Nagano 397-0101, Japan
(7) CREST, Indian Institute of Astrophysics, Hosakote 562 114, India
(8) Institute of Astronomy, National Central University, Jhongli 32001, Taiwan
(9) Centro de Investigaciones de Astronomía (CIDA), Apartado Postal 264, Mérida 5101-A, Venezuela
Accepted byPublication of the ASJ
Contactsaurabh@aries.res.in
URLhttp://arxiv.org/abs/1204.2897
Links IC 1590

Abstract

We present a multiwavelength study of the NGC 281 complex which contains the young cluster IC 1590 at the center, using deep wide-field optical $UBVI_c$ photometry, slitless spectroscopy along with archival data sets in the near-infrared (NIR) and X-ray. The extent of IC 1590 is estimated to be ~6.5 pc. The cluster region shows a relatively small amount of differential reddening. The majority of the identified young stellar objects (YSOs) are low mass PMS stars having age <1-2 Myr and mass 0.5-3.5 M(sun). The slope (Γ) of the mass function for IC 1590, in the mass range 2 < M/M(sun) ≤ 54, is found to be -1.11±0.15. The slope of the K-band luminosity function (0.37±0.07) is similar to the average value (~0.4) reported for young clusters. The distribution of gas and dust obtained from the IRAS, CO and radio maps indicates clumpy structures around the central cluster. The radial distribution of the young stellar objects, their ages, Δ(H-K) NIR-excess, and the fraction of classical T Tauri stars suggest triggered star formation at the periphery of the cluster region. However, deeper optical, NIR and MIR observations are needed to have a conclusive view of star formation scenario in the region. The properties of the Class 0/I and Class II sources detected by using the Spitzer mid-infrared observations indicate that a majority of the Class II sources are X-ray emitting stars, whereas X-ray emission is absent from the Class 0/I sources. The spatial distribution of Class 0/I and Class II sources reveals the presence of three sub-clusters in the NGC 281 West region.