2009A&A...508..645G


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.30CEST17:36:34

2009A&A...508..645G - Astronomy and Astrophysics, volume 508, 645-664 (2009/12-3)

Probing the dust properties of galaxies up to submillimetre wavelengths. I. The spectral energy distribution of dwarf galaxies using LABOCA.

GALAMETZ M., MADDEN S., GALLIANO F., HONY S., SCHULLER F., BEELEN A., BENDO G., SAUVAGE M., LUNDGREN A. and BILLOT N.

Abstract (from CDS):

We study the dust properties of four low metallicity galaxies by modelling their spectral energy distributions. This modelling enables us to constrain the dust properties such as the mass, the temperature or the composition to characterise the global ISM properties in dwarf galaxies. We present 870µm images of four low metallicity galaxies (NGC 1705, Haro 11, Mrk 1089 and UM 311) observed with the Large APEX BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope. We modeled their spectral energy distributions combining the submm observations of LABOCA, 2MASS, IRAS, Spitzer photometric data, and the IRS data for Haro 11. We found that the PAH mass abundance is very low in these galaxies, 5 to 50 times lower than the PAH mass fraction of our Galaxy. We also found that a significant mass of dust is revealed when using submm constraints compared to that measured with only mid-IR to far-IR observations extending only to 160 µm. For NGC 1705 and Haro 11, an excess in submillimeter wavelengths was detected when we used our standard dust SED model. We rerun our SED procedure adding a cold dust component (10K) to better describe the high 870 µm flux derived from LABOCA observations, which significantly improves the fit. We found that at least 70% of the dust mass of these two galaxies can reside in a cold dust component. We also showed that the subsequent dust-to-gas mass ratios, considering HI and CO observations, can be strikingly high for Haro 11 in comparison with what is usually expected for these low-metallicity environments. Furthermore, we derived the star formation rate of our galaxies and compared them to the Schmidt law. Haro 11 falls anomalously far from the Schmidt relation. These results may suggest that a reservoir of hidden gas could be present in molecular form not traced by the current CO observations. While there can be a significant cold dust mass found in Haro 11, the SED peaks at exceptionally short wavelengths (36µm), also highlighting the importance of the much warmer dust component heated by the massive star clusters in Haro 11. We also derived the total IR luminosities derived from our models and compared them with relations that derive this luminosity from Spitzer bands. We found that the Draine & Li (2007ApJ...657..810D) formula compares well to our direct IR determinations.

Abstract Copyright:

Journal keyword(s): galaxies: ISM - galaxies: dwarf - infrared: ISM - dust, extinction

Simbad objects: 29

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Number of rows : 29

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 QSO B0003-066 BLL 00 06 13.89288849 -06 23 35.3353162   19.1   17.14   ~ 264 1
2 NAME IC 10 NW MoC 00 20 17.7 +59 18 44           ~ 8 0
3 IC 10 G 00 20 23.16 +59 17 34.7   13.6 9.5     ~ 1013 0
4 ESO 350-38 AGN 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 292 0
5 QSO B0055-26 QSO 00 57 58.0249885733 -26 43 14.753717865   17.90 17.47 17.99   ~ 135 1
6 QSO B0104-408 QSO 01 06 45.10796851 -40 34 19.9602291   18.60 19.0 19.25   ~ 119 0
7 NGC 450 H2G 01 15 30.470 -00 51 38.98   13.4   13.3 13.2 ~ 204 0
8 UGC 807 GiP 01 15 35.003 -00 50 51.98   13.0       ~ 36 0
9 NGC 1140 EmG 02 54 33.5258827369 -10 01 43.135585379 12.41 12.84 12.49 13.6 13.5 ~ 263 1
10 SBSG 0335-052 bCG 03 37 44.04 -05 02 38.5     16.65     ~ 435 1
11 QSO J0403-3605 QSO 04 03 53.7499146834 -36 05 01.914911296   17.04 17.17 16.67   ~ 237 1
12 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1064 3
13 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1156 3
14 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1219 0
15 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
16 [CSW2006] D2 PoG 04 54 12.420 -53 21 45.07           ~ 3 0
17 NGC 1705 SBG 04 54 13.500 -53 21 39.82 12.32 12.96 12.56 12.58 12.9 ~ 598 1
18 [CSW2006] D1 PoG 04 54 14.590 -53 21 36.20           ~ 3 0
19 2MASX J05013782-0415294 G 05 01 37.832 -04 15 28.48   13.44   12.76   ~ 68 1
20 NGC 1741 IG 05 01 38.3 -04 15 25   13.7   13.02 13.6 ~ 250 0
21 2MASXI J0501387-041533 G 05 01 38.301 -04 15 33.91   15.62   14.43   ~ 23 0
22 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14950 1
23 V* V883 Ori Or* 05 38 18.0974260202 -07 02 25.963144400   14.80       F:I: 112 0
24 QSO B0537-441 BLL 05 38 50.36155219 -44 05 08.9389165   15.77 16.48 16   ~ 792 2
25 NAME NGC 2071 IR SFR 05 47 04.4 +00 21 49           ~ 62 0
26 UGCA 116 H2G 05 55 42.645 +03 23 32.23 10.74 11.68 11.46   11.82 ~ 501 0
27 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 506 3
28 NGC 4631 GiP 12 42 08.009 +32 32 29.44   9.78 9.19 9.10   ~ 975 2
29 NAME Local Group GrG ~ ~           ~ 7042 0

    Equat.    Gal    SGal    Ecl

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2020.09.30-17:36:34

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