2010A&A...514A..15O


Query : 2010A&A...514A..15O

2010A&A...514A..15O - Astronomy and Astrophysics, volume 514, A15-15 (2010/5-1)

Detection of unidentified infrared bands in a Hα filament in the dwarf galaxy NGC 1569 with AKARI.

ONAKA T., MATSUMOTO H., SAKON I. and KANEDA H.

Abstract (from CDS):

We report the detection of unidentified infrared (UIR) bands in a filamentary structure associated with Hα emission in the starburst dwarf galaxy NGC 1569 based on imaging and spectroscopic observations of the AKARI satellite. We investigate the processing and destruction of the UIR band carriers in an outflow from NGC 1569. We performed observations of NGC 1569 for 6 infrared bands (3.2, 4.1, 7, 11, 15, and 24µm) with the infrared camera (IRC) onboard AKARI. Near- to mid-infrared (2-13µm) spectroscopy of a Hα filament was also carried out with the IRC. The extended structure associated with a Hα filament appears bright at 7µm. Since the IRC 7µm band (S7) efficiently traces the 6.2 and 7.7µm UIR band emission, the IRC imaging observations suggest that the filament is bright at the UIR band emission. Follow-up spectroscopic observations with the IRC confirm the presence of 6.2, 7.7, and 11.3µm emission in the filament. The filament spectrum exhibits strong 11.3µm UIR band emission relative to the 7.7µm band compared to the galaxy disk observed with the infrared spectrograph on Spitzer. The near-infrared spectrum also suggests the presence of excess continuum emission in 2.5-5µm in the filament. The presence of the UIR bands associated with a Hα filament is found by AKARI/IRC observations. The Hα filament is thought to have been formed by the galactic outflow originating from the star-formation activity in the disk of NGC 1569. The destruction timescale of the UIR band carriers in the outflow is estimated to be much shorter (∼1.3x103yr) than the timescale of the outflow (∼5.3Myr). Thus it is unlikely that the band carriers survive the outflow environment. Alternatively, we suggest that the band carriers in the filaments may be produced by the fragmentation of large carbonaceous grains in shocks, which produce the Hα emission. The NIR excess continuum emission cannot be accounted for by free-free emission alone and a hot dust contribution may be needed, although the free-free emission intensity estimated from HI recombination lines has a large uncertainty.

Abstract Copyright:

Journal keyword(s): galaxies: ISM - infrared: galaxies - dust, extinction - galaxies: individual: NGC 1569

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3137 2
2 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1286 1
3 NAME IC 342 Group GrG 03 48 42 +68 00.8           ~ 99 1
4 NAME NGC 1569 CL* A Cl* 04 30 48.2 +64 50 59   15.45 15.22     ~ 100 1
5 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1198 3
6 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5606 6
7 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2379 2

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2022.06.30-11:45:56

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