2011A&A...533A.137K

Query : 2011A&A...533A.137K

2011A&A...533A.137K - Astronomy and Astrophysics, volume 533A137-137 (2011/9-1)

H2 flows in the Corona Australis Cloud and their driving sources.

KUMAR M.S.N., SHARMA S., DAVIS C.J., BORISSOVA J. and GRAVE J.M.C.

Abstract (from CDS):

We uncover the H2 flows in the Corona Australis molecular cloud and in particular identify the flows from the Coronet cluster. A deep, near-infrared H2 v=1-0 S(1), 2.122µm-line, narrow-band imaging survey of the R CrA cloud core was carried out. The nature of all candidate-driving sources in the region was evaluated using data available from the literature and also by fitting the spectral energy distributions (SED) of each source either with an extincted photosphere or YSO model. Archival Spitzer-IRAC and MIPS data was used to obtain photometry, which was combined with USNO, 2MASS catalogs and millimeter photometry from the literature, to build the SEDs. We identify the best candidate-driving source for each outflow by comparing the flow properties, available proper motions, and the known/estimated properties of the driving sources. We also adopted the thumbrule of outflow power as proportional to source luminosity and inversely proportional to the source age to reach a consensus. Continuum-subtracted, narrow-band images reveal several new Molecular Hydrogen emission-line Objects (MHOs). Together with previously known MHOs and Herbig-Haro objects we catalog at least 14 individual flow components of which 11 appear to be driven by the R CrA aggregate members. The flows originating in the Coronet cluster have lengths of ∼0.1-0.2pc. Eight out of nine submillimeter cores mapped in the Coronet cluster region display embedded stars driving an outflow component. Roughly 80% of the youngest objects in the Coronet are associated with outflows. The MHO flows to the west of the Coronet display lobes moving to the west and vice-versa, resulting in nondetections of the counter lobe in our deep imaging. We speculate that these counter flows may be experiencing a stunting effect in penetrating the dense central core. Although this work has reduced the ambiguities for many flows in the Coronet region, one of the brightest H2 feature (MHO2014) and a few fainter features in the region remain unassociated with a clear driving source. The flows from Coronet, therefore, continue to be interesting targets for future studies.

Abstract Copyright: ∼

Journal keyword(s): stars: formation - ISM: jets and outflows - stars: variables: T Tauri, Herbig Ae/Be - Herbig-Haro objects

Simbad objects: 69

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Number of rows : 69
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 1333 OpC 03 29 09.2 +31 20 59           ~ 1575 1
2 HD 176356 * 18 58 31.3115194368 +32 59 14.333729424   9.13 8.99     A 12 0
3 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 286 0
4 HH 729A HH 19 01 10.56 -36 57 32.4           ~ 9 0
5 HH 729B HH 19 01 12.94 -36 57 48.2           ~ 4 0
6 HH 729C HH 19 01 15.68 -36 57 56.4           ~ 4 0
7 HH 730C HH 19 01 15.72 -37 00 30.0           ~ 3 0
8 HH 730B HH 19 01 24.08 -36 59 59.8           ~ 3 0
9 HH 730A HH 19 01 25.26 -36 59 30.0           ~ 6 0
10 MHO 2005 EmO 19 01 28.879 -36 57 10.66           ~ 2 0
11 JCMTSF J190133.9-365334 mm 19 01 33.2 -36 53 35           ~ 6 0
12 MHO 2007 EmO 19 01 34.9 -37 02 56           ~ 2 0
13 HH 101S HH 19 01 34.93 -37 03 01.2           ~ 11 0
14 VSST 16 * 19 01 35.0 -37 02 58           ~ 3 0
15 HH 101N HH 19 01 35.09 -37 02 55.4           ~ 13 0
16 [FP2007] J190137.07-365601.9 X 19 01 37.07 -36 56 01.9           ~ 2 0
17 HD 176386 Or* 19 01 38.9318002416 -36 53 26.561166432 7.28 7.44 7.32 8.11   B9Vbs 149 0
18 MHO 2008 EmO 19 01 40.080 -37 00 02.97           ~ 3 0
19 V* TY CrA Ae* 19 01 40.8284458320 -36 52 33.816176040 10.03 9.92 9.39     B9e 301 0
20 MHO 2006 EmO 19 01 40.9 -36 58 47           ~ 2 0
21 HH 96 HH 19 01 41.31 -37 00 51.1           ~ 14 0
22 [TS84] IRS 2 Y*O 19 01 41.569 -36 58 31.23           K2 97 0
23 2MASS J19014164-3659528 Or* 19 01 41.6426330712 -36 59 52.868573844   17.7 16.7     M2 40 0
24 2MASS J19014190-3656585 Y*O 19 01 41.91 -36 56 58.6           ~ 9 0
25 HH 101 HH 19 01 42 -37 00.7           ~ 44 0
26 MHO 2004 EmO 19 01 45.5 -36 56 45           ~ 2 0
27 HH 97 HH 19 01 45.78 -37 00 01.5           ~ 15 0
28 [CKR2003] MMS 10 mm 19 01 45.9 -36 55 48           ~ 5 0
29 JCMTSF J190145.9-365533 smm 19 01 46.4 -36 55 30           ~ 6 0
30 2MASS J19014805-3657219 Y*O 19 01 48.056 -36 57 21.95           ~ 108 0
31 CHLT 3 * 19 01 48.10 -36 57 22.7           K6V 37 0
32 2MASS J19014846-3657148 Y*O 19 01 48.461 -36 57 14.88           ~ 34 0
33 HH 100 HH 19 01 49.1 -36 58 16           ~ 82 0
34 MHO 2003 EmO 19 01 50.0 -36 58 30           ~ 2 0
35 [TS84] IRS 6 Y*O 19 01 50.373 -36 56 39.05           M2 38 0
36 [TS84] IRS 6B * 19 01 50.63 -36 56 37.1           ~ 4 0
37 V* V710 CrA Or* 19 01 50.67792 -36 58 09.6132           K7: 131 0
38 NAME Corona Australis Cloud MoC 19 01 51 -36 58.9           ~ 554 0
39 [B92b] 30 Y*O 19 01 52.63 -36 57 00.2           ~ 31 0
40 V* R CrA Ae* 19 01 53.6764322232 -36 57 08.299341828 12.781 12.651 11.917 11.242 10.412 B5IIIpe 499 2
41 NAME Coronet Cluster Cl* 19 01 54 -36 57.2           ~ 106 1
42 [NWA2005] SMM 1C mm 19 01 55.28 -36 57 16.6           ~ 29 1
43 2MASS J19015545-3657231 Y*O 19 01 55.460 -36 57 23.13           ~ 105 2
44 [CKR2003] MMS 13 smm 19 01 55.5 -36 57 38           ~ 27 0
45 MHO 2015 EmO 19 01 56.0 +36 58 50           ~ 3 0
46 MHO 2016 EmO 19 01 56.0 +36 58 50           ~ 1 0
47 CHLT 14 Y*O 19 01 56.41 -36 57 28.0           ~ 121 1
48 HH 732B HH 19 01 56.41 -36 51 38.4           ~ 3 0
49 HH 732A HH 19 01 57.217 -36 52 08.52           ~ 5 0
50 HH 732C HH 19 01 57.73 -36 52 17.0           ~ 4 0
51 CHLT 15 Y*O 19 01 58.55 -36 57 08.7           ~ 28 0
52 2MASS J19015865-3656170 Y*? 19 01 58.6622273232 -36 56 17.099313792           ~ 21 0
53 V* T CrA Ae* 19 01 58.777008 -36 57 49.93704   14.087 13.130 11.823 10.678 F5? 179 0
54 MHO 2002 EmO 19 01 59.0 -36 57 15           ~ 2 0
55 HH 104 HH 19 01 59.090 -36 57 16.30           ~ 9 1
56 MHO 2014 EmO 19 02 00.6 -36 52 27           ~ 2 0
57 MHO 2001 EmO 19 02 01.0 -36 56 40           ~ 2 0
58 HH 99 HH 19 02 05.407 -36 54 39.85           ~ 29 0
59 HH 99A HH 19 02 05.41 -36 54 39.6           ~ 19 0
60 MHO 2000 EmO 19 02 05.561 -36 54 37.60           ~ 2 0
61 MHO 2013 EmO 19 02 09.4 -36 54 42           ~ 4 0
62 HH 733 HH 19 02 09.47 -36 54 46.2           ~ 6 0
63 HH 734A HH 19 02 11.01 -36 58 28.6           ~ 5 0
64 MHO 2009 EmO 19 02 12.3 -36 57 11           ~ 2 0
65 HH 735A HH 19 02 12.56 -36 56 37.8           ~ 5 0
66 MHO 2012 EmO 19 02 13.9 -36 56 06           ~ 2 0
67 MHO 2011 EmO 19 02 21.247 -36 55 53.97           ~ 2 0
68 HH 101B HH ~ ~           ~ 3 0
69 HH 101A HH ~ ~           ~ 4 0

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