Young Stellar Cluster in the Vicinity of the IRAS 05137+3919 Source

Abstract

PMS stellar objects are identified in a cluster located in the vicinity of IRAS 05137+3919 using the UKIDSS data base and Spitzer telescope (IRAC) images. The age of the cluster is 1.5-2.0 million years.Young stars are distributed nonuniformly in the cluster and form two subgroups. One is localized around the YSO CPM, which is a binary star, and the second contains a substantial number of objects with early spectral classes surrounded by gas-dust nebulae. The K luminosity functions of the PMS stars indicate that the cluster is at a distance of ~4.5 kpc. One of the components of CPM 15 appears to have Sp B3-B5 and is an Ae/Be Herbig star.

Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

“…However, the colour-colour diagram (J-H vs. H-K s ) of Nikoghosyan & Azatyan (2014) Salas (2007) is unlikely to apply to such objects. However, the presence of a spherical envelope around the disk should cause a greater decrease of H-K s for the same variation of K s , than in the case of a "naked" disk.…”

“…Indeed, despite the luminosity above 10 4 L , the source was not detected at 6 cm and 2 cm by Molinari et al (1998), while only weak, compact continuum emission (0.33 mJy; Molinari et al 2002) was measured at 3.6 cm. Whether this originates in an Hii region or in a thermal jet still needs to be understood, but it appears likely that the 3.6 cm continuum emission is associated with one of the members of the embedded stellar cluster detected in the near IR by various authors (Ishii et al 1998(Ishii et al , 2002Varricat et al 2010) and studied by Faustini et al (2009), Kumar et al (2006), and Nikoghosyan & Azatyan (2014, 2015. The most likely candidates for ionising the radio source are two bright stars located at the centre of the cluster and already identified by Varricat et al (2010).…”

Multiple Star Systems in the Young Cluster IRAS 05137+3919

“…These samples include, first of all, a list of 84 PMS objects identified as members of a cluster [12]. A search for close pairs increased this number to 88, or 76% of the excess number of objects relative to objects in the field near the cluster [12]; second, objects taken from the 2MASS survey (49 objects); and, third, stars taken from the UKIDSS survey with stellar magnitudes to 5 3 show plots of ) ( as a function of angular distance between the objects constructed using the 2PCF and TPACF functions, respectively. The two graphs show clearly that among the bright objects and PMS stars there is an excess of pairs (relative to a random distribution) at distances up to 0.6 arcsec.…”

“…We have determined the masses of these objects using the relationship between the absolute stellar magnitude and mass of young stars [19] for a cluster distance of 4.4 kpc and an absorption of A V = 1 m .8 [12]. The results are shown in Table 2.…”

“…In this paper we present the results of a study of multiple systems in a single cluster, specifically an R-association in the neighborhood of the IRAS 05137+3919 source [12]. The cluster has a radius of 1.5 ang.…”