2007A&A...466..509T


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.03CET18:44:59

2007A&A...466..509T - Astronomy and Astrophysics, volume 466, 509-519 (2007/5-1)

A multi-scale study of infrared and radio emission from Scd galaxy M 33.

TABATABAEI F.S., BECK R., KRAUSE M., BERKHUIJSEN E.M., GEHRZ R., GORDON K.D., HINZ J.L., HUMPHREYS R., McQUINN K., POLOMSKI E., RIEKE G.H. and WOODWARD C.E.

Abstract (from CDS):

We investigate the energy sources of the infrared(IR) emission and their relation to the radio continuum emission at various spatial scales within the Scd galaxy M 33. We use the data at the Spitzer wavelengths of 24, 70, and 160µm, as well as recent radio continuum maps at 3.6cm and 20cm observed with the 100-m Effelsberg telescope and VLA, respectively. We use the wavelet transform of these maps to a) separate the diffuse emission components from compact sources, b) compare the emission at different wavelengths, and c) study the radio-IR correlation at various spatial scales. An Hα map serves as a tracer of the star forming regions and as an indicator of the thermal radio emission. The bright HII regions affect the wavelet spectra causing dominant small scales or decreasing trends towards the larger scales. The dominant scale of the 70µm emission is larger than that of the 24µm emission, while the 160µm emission shows a smooth wavelet spectrum. The radio and Hα maps are well correlated with all 3 MIPS maps, although their correlations with the 160µm map are weaker. After subtracting the bright HII regions, the 24 and 70µm maps show weaker correlations with the 20cm map than with the 3.6cm map at most scales. We also find a strong correlation between the 3.6cm and Hα emission at all scales. Comparing the results with and without the bright HII regions, we conclude that the IR emission is influenced by young, massive stars increasingly with decreasing wavelength from 160 to 24µm. The radio-IR correlations indicate that the warm dust-thermal radio correlation is stronger than the cold dust-nonthermal radio correlation at scales smaller than 4kpc. A perfect 3.6cm-Hα correlation implies that extinction has no significant effect on Hα emitting structures.

Abstract Copyright:

Journal keyword(s): methods: data analysis - ISM: HII regions - galaxies: clusters: individual: M 33 - infrared: galaxies - radio continuum: galaxies

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

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 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11105 1
2 VGHC 1-1 Rad 01 31 57 +31 10.5           ~ 4 0
3 6W 0129+30W01 Rad 01 32 21 +30 44.0           ~ 7 0
4 6W 0129+30W02 Rad 01 32 29 +31 09.2           ~ 4 0
5 NGC 595 HII 01 33 33.53 +30 41 29.8           ~ 193 0
6 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5216 1
7 NGC 604 HII 01 34 32.1 +30 47 01           ~ 553 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15067 1
9 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2268 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2007A&A...466..509T and select 'bookmark this link' or equivalent in the popup menu


2020.12.03-18:44:59

© Université de Strasbourg/CNRS

    • Contact