2004A&A...418..563R


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.20CET15:24:51

2004A&A...418..563R - Astronomy and Astrophysics, volume 418, 563-576 (2004/5-1)

The giant pillars of the Carina Nebula.

RATHBORNE J.M., BROOKS K.J., BURTON M.G., COHEN M. and BONTEMPS S.

Abstract (from CDS):

Result. are presented from a multi-wavelength study of the giant pillars within the Carina Nebula. Using near-IR data from 2MASS, mid-IR data from MSX, 843MHz radio continuum maps from the MOST and molecular line and continuum observations from the SEST, we investigate the nature of the pillars and search for evidence of ongoing star formation within them. Photodissociation regions (PDRs) exist across the whole nebula and trace the giant pillars, as well as many ridges, filaments and condensations (Av>7mag). Morphological similarities between emission features at 21µm and 843MHz adjacent to the PDRs, suggests that the molecular material has been carved by the intense stellar winds and UV radiation from the nearby massive stars. In addition, star forming cores are found at the tips of several of the pillars. Using a stellar density distribution, several candidate embedded clusters are also found. One is clearly seen in the 2MASS images and is located within a dense core (G287.84-0.82). A search for massive young stellar objects and compact HII regions using mid-IR colour criteria, reveal twelve candidates across the complex. Grey-body fits to SEDs for four of these objects are suggestive of OB-stars. We find that massive star formation in the Carina Nebula is occurring across the whole complex and confirm it has been continuous over the past 3 Myrs.

Abstract Copyright:

Journal keyword(s): ISM: structure - ISM: lines and bands - ISM: molecules - HII regions - dust, extinction - stars: formation

Simbad objects: 32

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Number of rows : 32

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 Cl Bochum 10 OpC 10 42 14.2 -59 08 44   6.40 6.2     ~ 71 0
2 MSX6C G287.22-00.53 HII 10 42 49.2 -59 25 27           ~ 2 0
3 NAME Carina I HII Region HII 10 43 32 -59 35.0           ~ 50 0
4 MSX6C G287.57-00.91 HII 10 43 51.1 -59 55 23           ~ 3 0
5 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 417 0
6 MSX6C G287.68-01.09 HII 10 43 57.2 -60 08 25           ~ 1 0
7 Cl Collinder 228 OpC 10 44 00 -60 05.2   4.58 4.4     ~ 186 0
8 2MASX J10441798-6027447 Y*O 10 44 17.981 -60 27 44.73           B0 9 0
9 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 872 2
10 [RBB2002] N4 mul 10 44 32.1 -59 33 20           ~ 8 0
11 HD 93222 * 10 44 36.2479580459 -60 05 28.886871750 7.26 8.15 8.10 8.91   O7V((f))z 180 0
12 Cl Trumpler 15 OpC 10 44 43 -59 22.0   7.41 7.0     ~ 171 0
13 MSX6C G287.73-00.92 PoC 10 44 45.4 -59 59 16           ~ 3 0
14 NAME Car II HII Region HII 10 44 47 -59 38.8           ~ 35 0
15 [SEC2000] G287.73-0.92 IR 10 44 55 -60 00.2           ~ 2 0
16 MSX6C G287.51-00.49 HII 10 44 59.0 -59 31 24           ~ 4 0
17 IRAS 10430-5931 HII 10 45 02.4 -59 47 10           ~ 15 0
18 Cl Trumpler 16 OpC 10 45 10 -59 43.0   5.35 5.0     ~ 417 0
19 [MHL2007] G287.5233-00.4126 1 Y*? 10 45 20.60 -59 27 30.0           ~ 2 0
20 MSX6C G287.76-00.87 HII 10 45 22.3 -59 58 23           ~ 1 0
21 IRAS 10439-5941 HII 10 45 54.0 -59 57 03           ~ 12 0
22 MSX6C G287.93-00.99 PoC 10 45 56.1 -60 08 50           ~ 2 0
23 MSX6C G287.75-00.66 HII 10 46 01.2 -59 46 58           ~ 2 0
24 IRAS 10441-5949 HII 10 46 02.8 -60 05 31           ~ 4 0
25 [SEC2000] G287.84-0.82 Cl* 10 46 04 -59 58.0           ~ 4 1
26 [SEC2000] G287.93-0.99 IR 10 46 05 -60 09.5           ~ 2 0
27 MSX6C G287.86-00.82 IR 10 46 13.85 -59 58 41.3           ~ 1 0
28 MSX6C G287.80-00.56 * 10 46 46.6609532188 -59 43 26.429576596           ~ 1 0
29 C 1045-598 OpC 10 47 15.2 -60 05 51   8.16 7.9     ~ 67 0
30 MSX6C G288.07-00.80 PoC 10 47 35.4 -60 02 51           ~ 1 0
31 [SEC2000] G288.07-0.80 IR 10 47 47 -60 03.3           ~ 2 0
32 NGC 3606 GiG 11 16 15.645 -33 49 38.67   13.42   11.72   ~ 57 0

    Equat.    Gal    SGal    Ecl

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2020.01.20-15:24:51

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