Far‐Infrared Observations of the Galactic Star‐forming Regions Associated with IRAS 00338+6312 and RAFGL 5111

1999 ◽  
Vol 522 (1) ◽  
pp. 285-296 ◽  
Author(s):  
B. Mookerjea ◽  
S. K. Ghosh ◽  
A. D. Karnik ◽  
T. N. Rengarajan ◽  
S. N. Tandon ◽  
...  
Keyword(s):  
Far Infrared ◽  
Infrared Observations ◽  
Star Forming ◽  
Star Forming Regions

Far-infrared observations of star-forming regions

1981 ◽  
Vol 249 ◽  
pp. 607 ◽  
Author(s):  
A. I. Sargent ◽  
R. J. van Duinen ◽  
J. W. G. Aalders ◽  
C. V. M. Fridlund ◽  
H. L. Nordh
Keyword(s):  
Far Infrared ◽  
Infrared Observations ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

2020 ◽  
Vol 494 (2) ◽  
pp. 2823-2838 ◽  
Author(s):  
Ana Trčka ◽  
Maarten Baes ◽  
Peter Camps ◽  
Sharon E Meidt ◽  
James Trayford ◽  
...  
Keyword(s):  
Radiative Transfer ◽  
Physical Properties ◽  
Numerical Models ◽  
Far Infrared ◽  
Spectral Energy ◽  
Star Forming ◽  
Star Forming Regions ◽  
Global Emission ◽  
Galaxy Sample ◽  
Galaxy Population

ABSTRACT We compare the spectral energy distributions (SEDs) and inferred physical properties for simulated and observed galaxies at low redshift. We exploit UV-submillimetre mock fluxes of ∼7000 z = 0 galaxies from the EAGLE suite of cosmological simulations, derived using the radiative transfer code skirt. We compare these to ∼800 observed galaxies in the UV-submillimetre range, from the DustPedia sample of nearby galaxies. To derive global properties, we apply the SED fitting code cigale consistently to both data sets, using the same set of ∼80 million models. The results of this comparison reveal overall agreement between the simulations and observations, both in the SEDs and in the derived physical properties, with a number of discrepancies. The optical and far-infrared regimes, and the scaling relations based upon the global emission, diffuse dust, and stellar mass, show high levels of agreement. However, the mid-infrared fluxes of the EAGLE galaxies are overestimated while the far-UV domain is not attenuated enough, compared to the observations. We attribute these discrepancies to a combination of galaxy population differences between the samples and limitations in the subgrid treatment of star-forming regions in the EAGLE-skirt post-processing recipe. Our findings show the importance of detailed radiative transfer calculations and consistent comparison, and provide suggestions for improved numerical models.

Mid- to far-infrared mapping spectroscopy of galactic star-forming regions with ISO, spitzer, and AKARI

2008 ◽  
Vol 31 ◽  
pp. 191-192
Author(s):  
Y. Okada ◽  
T. Onaka ◽  
T. Miyata ◽  
Y.K. Okamoto ◽  
I. Sakon ◽  
...  
Keyword(s):  
Far Infrared ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals The Youngest Star-Forming Regions in Galaxies: Giant Compact HII Regions and Protoglobular Clusters?

2001 ◽  
Vol 205 ◽  
pp. 224-227
Author(s):  
Jean L. Turner
Keyword(s):  
Dwarf Galaxy ◽  
Hii Regions ◽  
Starburst Galaxies ◽  
Mid Infrared ◽  
Infrared Observations ◽  
Star Forming ◽  
Bolometric Luminosity ◽  
Star Forming Regions ◽  
Young Clusters ◽  
Compact Hii Regions

Subarcsecond radio and infrared observations reveal a class of luminous, obscured, optically thick HII regions associated with extremely large young clusters in nearby starburst galaxies. VLA images show bright radio nebulae with ne ∼ 104 cm−3, densities characteristic of young Galactic compact HII regions. Excitation of the nebulae requires the presence of several thousand O stars within regions of 1-10 pc extent, corresponding to clusters containing 105–106 stars. The compact nebulae are also bright in the mid-infrared, and can for significant fractions of not only the total IR luminosity, but also the total bolometric luminosity, of the parent galaxies. The prototype for these “supernebulae” is the large, obscured cluster in the dwarf galaxy NGC 5253.

scholarly journals Investigations of dust heating in M81, M83 and NGC 2403 with Herschel and Spitzer

2011 ◽  
Vol 7 (S284) ◽  
pp. 97-100
Author(s):  
George J. Bendo ◽  
Keyword(s):  
Star Formation ◽  
Flux Density ◽  
Near Infrared ◽  
Dust Emission ◽  
Far Infrared ◽  
Spectral Energy ◽  
Star Forming ◽  
Star Forming Regions ◽  
Star Formation Activity ◽  
Density Ratios

AbstractWe use Herschel Space Observatory and Spitzer Space Telescope 70-500 μm data along with ground-based optical and near-infrared data to understand how dust heating in the nearby face-on spiral galaxies M81, M83, and NGC 2403 is affected by the starlight from all stars and by the radiation from star-forming regions. We find that 70/160 μm flux density ratios tend to be more strongly influenced by star-forming regions. However, the 250/350 and 350/500 μm micron flux density ratios are more strongly affected by the light from the total stellar populations, suggesting that the dust emission at > 250 μm originates predominantly from a component that is colder than the dust seen at <160 μm and that is relatively unaffected by star formation activity. We conclude by discussing the implications of this for modelling the spectral energy distributions of both nearby and more distant galaxies and for using far-infrared dust emission to trace star formation.

scholarly journals UCHII regions in the Antennae

2006 ◽  
Vol 2 (S237) ◽  
pp. 476-476
Author(s):  
L. Snijders ◽  
L. J. Kewley ◽  
P. P. van der Werf ◽  
B. R. Brandl
Keyword(s):  
Emission Line ◽  
Spatial Resolution ◽  
Average Density ◽  
Physical Characteristics ◽  
Stellar Clusters ◽  
Mid Infrared ◽  
Infrared Observations ◽  
Star Forming ◽  
Compact Material ◽  
Star Forming Regions

AbstractWe explore the physical characteristics of young stellar clusters in the Antennae by combining recent ground- and space-based mid-infrared observations with a newly developed set of diagnostic diagrams. Spitzer data give an overview of the star-forming regions extending over hundreds of parsecs, showing a dominant diffuse ISM component with a density of 102 cm−3 plus a small fraction of very compact material (106 cm−3). With its higher spatial resolution VISIR gives a close-up view of the latter component. Its emission line ratios suggest that these regions are fundamentally different from local star-forming regions. Instead of having small isolated UCHII regions, as in local star-forming regions, the average density of the medium of the whole region falls in the (ultra)compact regime, exceeding 104 cm−3 over tens of parsecs.

scholarly journals Far-infrared molecular lines from low- to high-mass star forming regions observed withHerschel

2014 ◽  
Vol 562 ◽  
pp. A45 ◽  
Author(s):  
A. Karska ◽  
F. Herpin ◽  
S. Bruderer ◽  
J. R. Goicoechea ◽  
G. J. Herczeg ◽  
...  
Keyword(s):  
Far Infrared ◽  
High Mass ◽  
Mass Star ◽  
Star Forming ◽  
Star Forming Regions ◽  
Molecular Lines

scholarly journals Probing star formation and ISM properties using galaxy disk inclination

2018 ◽  
Vol 615 ◽  
pp. A7 ◽  
Author(s):  
S. K. Leslie ◽  
M. T. Sargent ◽  
E. Schinnerer ◽  
B. Groves ◽  
A. van der Wel ◽  
...  
Keyword(s):  
Sample Selection ◽  
Ultra Violet ◽  
Far Infrared ◽  
Sloan Digital Sky Survey ◽  
Star Forming ◽  
Star Forming Regions ◽  
Sky Survey ◽  
Dust Fraction ◽  
Galaxy Disk ◽  
Intermediate Redshift

Disk galaxies at intermediate redshift (z ~ 0.7) have been found in previous work to display more optically thick behaviour than their local counterparts in the rest-frame B-band surface brightness, suggesting an evolution in dust properties over the past ~6 Gyr. We compare the measured luminosities of face-on and edge-on star-forming galaxies at different wavelengths (Ultraviolet (UV), mid-infrared (MIR), far-infrared (FIR), and radio) for two well-matched samples of disk-dominated galaxies: a local Sloan Digital Sky Survey (SDSS)-selected sample at z ~ 0.07 and a sample of disks at z ~ 0.7 drawn from Cosmic Evolution Survey (COSMOS). We have derived correction factors to account for the inclination dependence of the parameters used for sample selection. We find that typical galaxies are transparent at MIR wavelengths at both redshifts, and that the FIR and radio emission is also transparent as expected. However, reduced sensitivity at these wavelengths limits our analysis; we cannot rule out opacity in the FIR or radio. Ultra-violet attenuation has increased between z ~ 0 and z ~ 0.7, with the z ~ 0.7 sample being a factor of ~3.4 more attenuated. The larger UV attenuation at z ~ 0.7 can be explained by more clumpy dust around nascent star-forming regions. There is good agreement between the fitted evolution of the normalisation of the SFRUV versus 1 − cos(i) trend (interpreted as the clumpiness fraction) and the molecular gas fraction/dust fraction evolution of galaxies found out to z < 1.

scholarly journals On the origin of X-ray oxygen emission lines in obscured AGN

2020 ◽  
Vol 499 (4) ◽  
pp. 5107-5120
Author(s):  
V Reynaldi ◽  
M Guainazzi ◽  
S Bianchi ◽  
I Andruchow ◽  
F García ◽  
...  
Keyword(s):  
Far Infrared ◽  
Emission Lines ◽  
X Rays ◽  
X Ray ◽  
Star Forming ◽  
Star Forming Regions ◽  
Model Predictions ◽  
Ionization Model ◽  
Collisional Ionization ◽  
Shed Light

ABSTRACT We present the Catalogue of High Resolution Spectra of Obscured Sources (CHRESOS) from the XMM–Newton Science Archive. It comprises the emission-line luminosities of H- and He-like transitions from C to Si, and the Fe 3C and Fe 3G L-shell ones. Here, we concentrate on the soft X-ray O vii (f) and O viii Lyα emission lines to shed light on to the physical processes with which their formation can be related to active galactic nucleus (AGN) versus star-forming regions. We compare their luminosity with that of two other important oxygen key lines [O iii] λ5007 Å, in the optical, and [O iv] 25.89 μm, in the infrared (IR). We also test O vii (f) and O viii Lyα luminosities against that of continuum bands in the IR and hard X-rays, which point to different ionization processes. We probe into those processes by analysing photoionization and collisional ionization model predictions upon our lines. We show that both scenarios can explain the formation and observed intensities of O vii (f) and O viii Lyα. By analysing the relationships between O vii (f) and O viii Lyα, and all other observables: [O iii] λ5007 Å, [O iv] 25.89 μm emission lines, and mid-infrared (MIR) 12 μm, far-infrared (FIR) 60 and 100 μm, 2–10 and 14–195 keV continuum bands, we conclude that the AGN radiation field is mainly responsible of the soft X-ray oxygen excitation.

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