2010A&A...517A..27M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.23CET00:42:55

2010A&A...517A..27M - Astronomy and Astrophysics, volume 517, A27-27 (2010/7-1)

A study of the interplay between ionized gas and star clusters in the central region of NGC 5253 with 2D spectroscopy.

MONREAL-IBERO A., VILCHEZ J.M., WALSH J.R. and MUNOZ-TUNON C.

Abstract (from CDS):

Starbursts are one of the main contributors to the chemical enrichment of the interstellar medium. However, mechanisms governing the interaction between the recent star formation and the surrounding gas are not fully understood. Because of their a priori simplicity, the subgroup of HII galaxies constitute an ideal sample to study these mechanisms. A detailed 2D study of the central region of NGC 5253 has been performed to characterize the stellar and ionized gas structure as well as the extinction distribution, physical properties and kinematics of the ionized gas in the central ∼210pcx130pc. We utilized optical integral field spectroscopy (IFS) data obtained with FLAMES. A detailed extinction map for the ionized gas in NGC 5253 shows that the largest extinction is associated with the prominent Giant HII region. There is an offset of ∼0.5" between the peak of the optical continuum and the extinction peak in agreement with findings in the infrared. We found that stars suffer less extinction than gas by a factor of ∼0.33. The [SII]λ6717/[SII]λ6731 map shows an electron density (Ne) gradient declining from the peak of emission in Hα (790cm–3) outwards, while the argon line ratio traces areas with Ne∼4200-6200cm–3. The area polluted with extra nitrogen, as deduced from the excess [NII]λ6584/Hα, extends up to distances of 3.3" (∼60pc) from the maximum pollution, which is offset by ∼1.5" from the peak of continuum emission. Wolf-Rayet features are distributed in an irregular pattern over a larger area (∼100 pcx100 pc) and associated with young stellar clusters. We measured He+ abundances over most of the field of view and values of He++/H+≲0.0005 in localized areas which do not coincide, in general, with the areas presenting W-R emission or extra nitrogen. The line profiles are complex. Up to three emission components were needed to reproduce them. One of them, associated with the giant HII region, presents supersonic widths and [NII]λ6584 and [SII]λλ6717,6731 emission lines shifted up to 40km/s with respect to Hα. Similarly, one of the narrow components presents offsets in the [NII]λ6584 line of ≲20km/s. This is the first time that maps with such velocity offsets for a starburst galaxy have been presented. The observables in the giant HII region fit with a scenario where the two super stellar clusters (SSCs) produce an outflow that encounters the previously quiescent gas. The south-west part of the FLAMES IFU field is consistent with a more evolved stage where the star clusters have already cleared out their local environment.

Abstract Copyright:

Journal keyword(s): galaxies: starburst - galaxies: dwarf - galaxies: individual: NGC 5253 - galaxies: ISM - galaxies: abundances - galaxies: kinematics and dynamics

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 QSO B0125-0635 QSO 01 27 35.5241670251 -06 19 35.428005150 14.75 15.05 14.48 14.06 13.70 ~ 91 0
2 NGC 1450 G 03 45 36.630 -09 14 05.64   14.56       ~ 11 0
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15122 1
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5685 4
5 M 42 HII 05 35 17.3 -05 23 28           ~ 3765 0
6 NGC 4449 EmG 12 28 11.118 +44 05 36.81 10.11 9.98 9.64 9.45   ~ 1034 1
7 NGC 4485 GiP 12 30 31.113 +41 42 04.22 12.10 12.42 11.93 11.93   ~ 257 2
8 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4055 3
9 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2269 2
10 [LP2006] N5253-S001 SR? 13 39 55.37 -31 38 29.9           ~ 2 0
11 [LP2006] N5253-S002 SR? 13 39 55.47 -31 38 27.7           ~ 2 0
12 [DAZ2013] 38 Cl* 13 39 55.53 -31 38 29.7           ~ 17 0
13 [DAZ2013] 45 Cl* 13 39 55.58 -31 38 29.4           ~ 14 0
14 [HCG2004] NGC 5253 C 21 Cl* 13 39 55.83 -31 38 27.1           ~ 3 0
15 [HCG2004] NGC 5253 C 6 Cl* 13 39 55.87 -31 38 26.9           ~ 2 0
16 KSRWR HII-2 H2G 13 39 55.9 -31 38 24           ~ 25 0
17 [HCG2004] NGC 5253 C 24 Cl* 13 39 55.92 -31 38 27.0           ~ 2 0
18 [HCG2004] NGC 5253 C 20 Cl* 13 39 55.92 -31 38 24.6           ~ 2 0
19 [HCG2004] NGC 5253 C 25 Cl* 13 39 55.94 -31 38 28.2           ~ 2 0
20 [HCG2004] NGC 5253 C 13 Cl* 13 39 55.94 -31 38 22.1           ~ 2 0
21 [DAZ2013] 129 Cl* 13 39 55.98 -31 38 31.9           ~ 22 0
22 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1278 4
23 KSRWR HII-1 H2G 13 39 56.00 -31 38 25.8           ~ 17 0
24 NAME NGC 5353 Radio Supernebula Cl* 13 39 56.007 -31 38 25.00           ~ 47 0
25 [HCG2004] NGC 5253 C 8 Cl* 13 39 56.0169 -31 38 27.422           ~ 5 0
26 [HCG2004] NGC 5253 C 4 H2G 13 39 56.020 -31 38 27.89           ~ 32 0
27 [HCG2004] NGC 5253 C 23 Cl* 13 39 56.26 -31 38 26.2           ~ 2 0
28 CD-32 9927 * 14 11 46.3240134300 -33 03 14.379335532   10.793 10.444 10.12 10.106 A4 85 0
29 [STT2001] C2 Cl* 15 34 57.08 +23 30 06.5   21.53       ~ 4 0
30 [ATB2004] C2 Cl* ~ ~           ~ 8 0

    Equat.    Gal    SGal    Ecl

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2021.01.23-00:42:55

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