2012A&A...540A..83T


C.D.S. - SIMBAD4 rel 1.7 - 2020.04.08CEST04:25:06

2012A&A...540A..83T - Astronomy and Astrophysics, volume 540A, 83-83 (2012/4-1)

Spitzer observations of NGC 2264: the nature of the disk population.

TEIXEIRA P.S., LADA C.J., MARENGO M. and LADA E.A.

Abstract (from CDS):

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. 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. We build NIR dust extinction maps of the molecular cloud associated with the cluster, and determine it to have a mass of 2.1x103M above an AV of 7mag. Using a differential Ks-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 3.6µm to 8µm and on the 24µm 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 sub-clusterings, whereas sources with anaemic disks do not. Furthermore, sources with anaemic disks are found to be unembedded (i.e., with AV<3mag), whereas the clustered sources with thick disks are still embedded within the parental cloud. 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).

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: formation - ISM: clouds

Status at CDS:  

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 IC 348 OpC 03 44 34 +32 09.8           ~ 1216 1
2 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2949 0
3 V* DH Tau TT* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 261 0
4 V* DM Tau TT* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 499 0
5 V* GM Aur TT* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 545 0
6 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1946 1
7 NAME sigma Orionis Cluster MGr 05 38 42 -02 36.0           ~ 481 0
8 NAME Mon I MoC 06 35 +10.1           ~ 209 0
9 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1572 1
10 * 15 Mon Be* 06 40 58.65963 +09 53 44.7229 3.360 4.400 4.640   4.88 O7V+B1.5/2V 743 0
11 IRAS 06382+0939 Y*O 06 41 02.81160 +09 36 16.1712         19.89 ~ 74 0
12 RAFGL 989 Y*O 06 41 10.1592954288 +09 29 33.635497596   17.4 16.8 18.26 17.28 B2 238 0
13 NGC 2362 OpC 07 18 41 -24 57.3     4.1     ~ 360 0
14 NGC 2419 GlC 07 38 08.51 +38 52 54.9     10.05     ~ 801 0
15 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1496 1
16 NAME Cha II MoC 12 54 -77.2           ~ 295 0
17 NAME Lup Cloud SFR 16 03 -38.1           ~ 501 0
18 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2984 0
19 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 901 2
20 NAME Coronet Cluster Cl* 19 01 54 -36 57.2           ~ 80 1
21 IC 1396 OpC 21 39 00 +57 29.4           ~ 444 1
22 NGC 7790 OpC 23 58 24 +61 12.5   9.18 8.5     ~ 245 0

    Equat.    Gal    SGal    Ecl

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2020.04.08-04:25:06

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