2015
DOI: 10.1051/0004-6361/201525953
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Infrared emission of young HII regions: aHerschel/Hi-GAL study

Abstract: Context. Investigating the relationship between radio and infrared emission of Hii regions may help shed light on the nature of the ionizing stars and the formation mechanism of early-type stars in general. Aims. We have taken advantage of recent unbiased surveys of the Galactic plane such as Herschel/Hi-GAL and VLA/CORNISH to study a bona fide sample of young Hii regions located in the Galactic longitude range 10 • -65 • by comparing the mid-and far-IR continuum emission to the radio free-free emission at 5 G… Show more

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Cited by 36 publications
(67 citation statements)
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References 42 publications
(55 reference statements)
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“…associated with a Hii free-free CORNISH radio source (Cesaroni et al 2015), the magenta asterisks in Fig. 9, are consistently found in the same region covered by the cluster models hosting a B0.5 ZAMS star or earlier.…”
Section: Integrated Properties and Evolutionary Diagnosticsmentioning
confidence: 53%
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“…associated with a Hii free-free CORNISH radio source (Cesaroni et al 2015), the magenta asterisks in Fig. 9, are consistently found in the same region covered by the cluster models hosting a B0.5 ZAMS star or earlier.…”
Section: Integrated Properties and Evolutionary Diagnosticsmentioning
confidence: 53%
“…Models in which there are at least 3 ZAMS stars earlier than B0.5 are indicated by the yellow dots. The cyan and magenta straight lines are from Molinari et al (2016c), and the magenta stars represent the position occupied by the dense clumps in the Hi-GAL clump catalogue (Elia et al 2017) with a Hii region counterpart from Cesaroni et al (2015). The black lines represent the evolutionary tracks from Molinari et al (2008), together with the location of Hii regions from the same work.…”
Section: Integrated Properties and Evolutionary Diagnosticsmentioning
confidence: 96%
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“…The former is very sensitive to the temperature of the clump enshrouding the star forming region, as the typical spectral energy distribution of high-mass YSOs peaks around ∼100 µm (see e.g. van der Tak 2000; Cesaroni et al 2015). Since the environment is progressively heated by the newly formed stars, an increase in the dust temperature with time and thus an increase in T c [160−70] with age is expected.…”
Section: Target Selection and Characterizationmentioning
confidence: 99%
“…In a recent study, Cesaroni et al (2015; hereafter C2015) have compared N Ly to L bol for the sample of compact and ultracompact H ii regions identified by Purcell et al (2013) in the CORNISH survey (Hoare et al 2012). The value of L bol has been estimated for 200 objects by reconstructing the corresponding spectral energy distributions using the far-IR images of the Herschel/Hi-GAL survey of the Galactic plane (Molinari et al 2010) and ancillary data from 1 mm to the mid-IR.…”
Section: Introductionmentioning
confidence: 99%