Young stellar objects in the Monoceros OB1 molecular cloud

Margulis, M.; Lada, Charles J.; Young, Erick T.

doi:10.1086/167960

Cited by 45 publications

(58 citation statements)

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“…The near-infrared colors and emission and absorption features, long-wavelength continuum fluxes, and H 2 column densities lead to estimates of the visual extinction, A V , in the range from !20 to well over 100 mag (Thompson & Tokunaga 1978;Schwartz et al 1985;Chini et al 1986;Krügel et al 1987;Walker et al 1990;Schreyer et al 1997). Estimates of the source luminosity ($3000 L ), based on far-infrared, submillimeter, and radio measurements, are consistent with that of an early B star (Harvey et al 1977;Schwartz et al 1985;Chini et al 1986;Margulis et al 1989;Henning et al 1990). However, as all the measurements at long wavelengths were made with very large beams, they must have included a significant contribution of emission from the nearby submillimeter cluster mapped by Ward- Thompson et al (2000).…”

Section: Introductionsupporting

confidence: 54%

X‐Ray and Infrared Observations of Embedded Young Stars in NGC 2264

Simon

Dahm

2005

ApJ

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Images of the NGC 2264 star-forming region, which we have acquired with the XMM-Newton spacecraft, reveal strong X-ray emission from three deeply embedded (A V ! 10 mag) young stellar objects in the vicinity of Allen's infrared source (AFGL 989 = IRS 1) and Castelaz & Grasdalen's infrared source (RNO-EW = IRS 2). Thermal plasma models for the brightest source in X-rays, located 11 00 southwest of Allen's star, yield a quasi-steady luminosity of L X ¼ 10 33 ergs s À1 and an extraordinarily high X-ray temperature of 100 MK. The high temperature is consistent with the presence of emission lines of Fe xxv and Fe xxvi at photon energies of 6.7 and 6.9 keV, respectively. An even higher temperature of nearly $140 MK was observed during the rise phase of a powerful impulsive X-ray flare of another young star in the IRS 2 region. Moderate-resolution near-infrared (1-4 m) spectra of the embedded objects, obtained at the NASA Infrared Telescope Facility, exhibit deep water ice absorption bands, as well as a variety of emission and absorption features of H i, CO, and both neutral and ionized metals.

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Section: Introductionsupporting

confidence: 54%

X‐Ray and Infrared Observations of Embedded Young Stars in NGC 2264

Simon

Dahm

2005

ApJ

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“…The oldest members of the cluster are ∼5 Myr old (Dahm & Simon 2005), although there is significant observational evidence of ongoing star formation such as CO outflows (e.g. Margulis et al 1988), Herbig-Haro objects (Reipurth et al 2004), and luminous far-infrared sources detected by the Infrared Astronomical Satellite (Margulis et al 1989). The PMS population has furthermore been associated with X-ray emission (Flaccomio et al 2006) and active accretion (Hα observations, Dahm & Simon 2005;Fűrész et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Spitzerobservations of NGC 2264: the nature of the disk population

Teixeira

Lada

Marengo

et al. 2012

A&A

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Aims. NGC 2264 is a young cluster with a rich circumstellar disk population which makes it an ideal target for studying the evolution of stellar clusters. Our goal is to study the star formation history of NGC 2264 and to analyse the primordial disk evolution of its members. Methods. The study presented is based on data obtained with the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS) on board the Spitzer Space Telescope, combined with deep near-infrared (NIR) ground-based FLAMINGOS imaging and previously published optical data. Results. We build NIR dust extinction maps of the molecular cloud associated with the cluster, and determine it to have a mass of 2.1 × 10 3 M above an A V of 7 mag. Using a differential K s -band luminosity function (KLF) of the cluster, we estimate the size of the population of NGC 2264, within the area observed by FLAMINGOS, to be 1436 ± 242 members. The star formation efficiency is ≥∼25%. We identify the disk population and divide it into 3 groups based on their spectral energy distribution slopes from 3.6 μm to 8 μm and on the 24 μm excess emission: (i) optically thick inner disks, (ii) anaemic inner disks, and (iii) disks with inner holes, or transition disks. We analyse the spatial distribution of these sources and find that sources with thick disks segregate into subclusterings, whereas sources with anaemic disks do not. Furthermore, sources with anaemic disks are found to be unembedded (i.e., with A V < 3 mag), whereas the clustered sources with thick disks are still embedded within the parental cloud. Conclusions. NGC 2264 has undergone more than one star-forming event, where the anaemic and extincted thick disk population appear to have formed in separate episodes: the sources with anaemic disks are more evolved and have had time to disperse and populate a halo of the cluster. We also find tentative evidence of triggered star-formation in the Fox Fur Nebula. In terms of disk evolution, our findings support the emerging disk evolution paradigm of two distinct evolutionary paths for primordial optically thick disks: a homologous one where the disk emission decreases uniformly at NIR and mid-infrared (MIR) wavelengths, and a radially differential one where the emission from the inner region of the disk decreases more rapidly than from the outer region (forming transition disks).

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“…IRAS sources 06377+1020, 06380+1012, 06382+1017, and the discrete IRAS source 24 identified by Margulis, Lada, & Young (1989) are located within a radius of 10 0 from HH 575B. On the basis of their relative locations, none of these IRAS sources are likely to be the driving sources of HH 575.…”

Section: Discussionmentioning

confidence: 95%

“…An unbiased survey of the entire cloud for high-velocity molecular gas revealed five CO molecular outflows in the region (Margulis & Lada 1986;Margulis, Lada, & Snell 1988). By filtering the co-added maps of emission at 12, 25, 60, and 100 lm from the IRAS data, Margulis, Lada, & Young (1989) identified 30 discrete IRAS (25 lm) sources. Eighteen of these IRAS sources were found to have class I energy distributions, characteristic of deeply embedded protostellar objects.…”

Section: Introductionmentioning

confidence: 99%

Herbig-Haro Objects in the Monoceros OB1 Molecular Cloud

Wang

Yang

Wang

et al. 2003

The Astronomical Journal

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We carried out a wide-field [S ii]-emission imaging of the Monoceros OB1 molecular cloud (NGC 2264) to investigate the star formation and outflow activity of the region. Our narrowband [S ii] imaging covers an area of sky of $2 deg 2 , including the entire Mon OB1 cloud. In the northern part of the cloud two new Herbig-Haro (HH) objects, HH 572 and HH 575, are discovered. All four of the previously known HH objects, HH 124, 125, 225, and 226, are also detected in our imaging. Low-dispersion spectroscopic observations of HH 572A, 575B, and 575C1 further confirmed the HH-object nature of these objects. Molecular hydrogen v = 1-0 S(1) narrowband imaging revealed a bright H 2 emission knot in each of the HH 572 and HH 575 regions. By comparing the results of our optical [S ii] emission survey with those of the CO molecular outflow survey, it is found that the occurrence frequency of HH objects is similar to that of CO outflows in the Mon OB1 cloud. However, HH objects and CO outflows display different spatial distributions.

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Young stellar objects in the Monoceros OB1 molecular cloud

Cited by 45 publications

References 0 publications

X‐Ray and Infrared Observations of Embedded Young Stars in NGC 2264

X‐Ray and Infrared Observations of Embedded Young Stars in NGC 2264

Spitzerobservations of NGC 2264: the nature of the disk population

Herbig-Haro Objects in the Monoceros OB1 Molecular Cloud

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