2007A&A...467...93B


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.04CEST04:45:06

2007A&A...467...93B - Astronomy and Astrophysics, volume 467, 93-106 (2007/5-3)

Polychromatic view of intergalactic star formation in NGC 5291.

BOQUIEN M., DUC P.-A., BRAINE J., BRINKS E., LISENFELD U. and CHARMANDARIS V.

Abstract (from CDS):

Star formation (SF) takes place in unusual places such as way out in the intergalactic medium out of material expelled from parent galaxies. Whether SF proceeds in this specific environment in a similar way than in galactic disks is the question we wish to answer. Particularly, we address the reliability of ultraviolet, Hα and mid-infrared as tracers of SF in the intergalactic medium. We have carried out a multiwavelength analysis of the interacting system NGC 5291, which is remarkable for its extended HI ring hosting numerous intergalactic HII regions. We combined new ultraviolet (GALEX) observations with archival Hα, 8µm (Spitzer Space Telescope) and HI (VLA B-array) images of the system. We have found that the morphology of the star forming regions, as traced by the ultraviolet, Hα, and 8µm emission is similar. The 8.0µm infrared emission, normalised to emission from dust at 4.5µm, which is known to be dominated by PAH bands, is comparable to the integrated emission of dwarf galaxies of the same metallicity and to the emission of individual HII regions in spirals. The 8.0µm in the intergalactic environment is therefore an estimator of the star formation rate which is as reliable in that extreme environment as it is for spirals. There is a clear excess of ultraviolet emission compared to individual HII regions in spirals, i.e. the [8.0]/[NUV] and [Hα]/[NUV] SFR ratios are on average low although there are some large variations from one region to another, which cannot be explained by variations of the metallicity or the dust extinction along the HI structure. Comparing the observed SFR with a model of the evolution of [Hα]/[NUV] with time favours young, quasi-instantaneous though already fading starbursts. The total star formation rate measured in the intergalactic medium (which accounts for 80% of the total) surrounding NGC 5291 is up to 1.3M/yr - a value typical for spirals - assuming the standard SFR calibrations are valid. The SFR drops by a factor of 2 to 4 in case the star formation is indeed quasi-instantaneous.

Abstract Copyright:

Journal keyword(s): galaxies: individual: NGC 5291 - stars: formation - HII regions - intergalactic medium

Nomenclature: Fig.3, Table 1: [BDB2007] NN (Nos 1-29) = [BDB2007] GALEX JHHMMSS.ss+DDMMSS.ss N=32.

Simbad objects: 42

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Number of rows : 42

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 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14863 1
2 NGC 2535 rG 08 11 13.484 +25 12 24.97   13.5 12.60     ~ 162 0
3 APG 82 PaG 08 11 14.0 +25 12 25           ~ 144 0
4 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 3970 5
5 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3791 4
6 NAME Seashell G 13 44.5 -30 10           ~ 10 0
7 [BDB2007] GALEX J134700.56-302518.62 UV 13 47 00.560 -30 25 18.62           ~ 1 0
8 2MASX J13471278-3027250 GiC 13 47 12.7259778370 -30 27 24.517677041   15.49       ~ 7 0
9 [BDB2007] GALEX J134717.07-302035.59 UV 13 47 17.070 -30 20 35.59           ~ 1 0
10 [BDB2007] GALEX J134717.57-302821.11 UV 13 47 17.570 -30 28 21.11           ~ 1 0
11 [BDB2007] GALEX J134717.69-302018.20 UV 13 47 17.690 -30 20 18.20           ~ 1 0
12 [BDB2007] GALEX J134717.79-302634.82 UV 13 47 17.790 -30 26 34.82           ~ 1 0
13 [DM98] Knot k G 13 47 17.810 -30 19 58.85   20.61 20.21     ~ 4 0
14 [BDB2007] GALEX J134717.91-302121.48 ISM 13 47 17.910 -30 21 21.48   20.03 19.76     ~ 4 0
15 [BDB2007] GALEX J134717.92-302158.54 G 13 47 17.920 -30 21 58.54   21.32 21.00     ~ 4 0
16 [BDB2007] GALEX J134717.97-302031.99 UV 13 47 17.970 -30 20 31.99           ~ 1 0
17 [BDB2007] GALEX J134718.08-302150.30 G 13 47 18.080 -30 21 50.30           ~ 2 0
18 [BDB2007] GALEX J134718.18-302042.76 UV 13 47 18.180 -30 20 42.76           ~ 1 0
19 [BDB2007] GALEX J134719.74-302025.73 G 13 47 19.740 -30 20 25.73   20.27 20.01     ~ 6 0
20 [BDB2007] GALEX J134719.76-302648.77 UV 13 47 19.760 -30 26 48.77           ~ 1 0
21 LEDA 718304 GiG 13 47 20.5 -30 20 54   18.27 17.91     ~ 24 0
22 [BDB2007] GALEX J134720.69-302642.66 PoG 13 47 20.690 -30 26 42.66           ~ 2 0
23 [BDB2007] GALEX J134720.94-302131.97 UV 13 47 20.940 -30 21 31.97           ~ 1 0
24 [BDB2007] GALEX J134721.02-302311.33 HI 13 47 21.020 -30 23 11.33           ~ 1 0
25 [BDB2007] GALEX J134721.14-302026.07 UV 13 47 21.140 -30 20 26.07           ~ 1 0
26 [BDB2007] GALEX J134721.66-302041.66 UV 13 47 21.660 -30 20 41.66           ~ 1 0
27 UGC 8717 G 13 47 22.196 +30 20 00.94   14.8       ~ 19 0
28 SLSBG 278 G 13 47 22.470 -30 21 44.13   19.85 19.39     ~ 6 0
29 [BDB2007] GALEX J134722.91-302750.19 UV 13 47 22.910 -30 27 50.19           ~ 1 0
30 [BDL2001] NGC 5291S GiG 13 47 23.0 -30 27 30           ~ 12 0
31 [BDB2007] GALEX J134723.00-302724.31 HII 13 47 23.000 -30 27 24.31   18.87 18.63     ~ 6 0
32 NAME the Seashell GiC 13 47 23.1858909795 -30 25 04.193208472   16   13.62   ~ 24 1
33 [BDB2007] GALEX J134723.37-302524.51 UV 13 47 23.370 -30 25 24.51           ~ 1 0
34 [BDB2007] GALEX J134723.86-302646.25 G 13 47 23.860 -30 26 46.25   21.88 21.65     ~ 4 0
35 [BDB2007] GALEX J134723.95-302622.21 PoG 13 47 23.950 -30 26 22.21   20.17 19.69     ~ 6 0
36 NGC 5291 AGN 13 47 24.459 -30 24 25.03   15.18 14.00 13.57 12.7 ~ 141 1
37 [BDB2007] GALEX J134724.51-302635.91 UV 13 47 24.510 -30 26 35.91           ~ 1 0
38 [BDB2007] GALEX J134726.10-302602.63 UV 13 47 26.100 -30 26 02.63           ~ 1 0
39 [BDB2007] 12 PoG 13 47 26.450 -30 25 45.78           ~ 1 0
40 [BDB2007] GALEX J134726.66-302552.06 PoG 13 47 26.660 -30 25 52.06   19.43 18.91     ~ 6 0
41 [BDB2007] GALEX J134727.77-302504.89 AGN 13 47 27.770 -30 25 04.89           ~ 2 0
42 NAME IC 4329 Group GrG 13 48 36.4 -30 30 13           ~ 132 2

    Equat.    Gal    SGal    Ecl

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2020.08.04-04:45:06

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