The JCMT Nearby Galaxies Legacy Survey - III. Comparisons of cold dust, polycyclic aromatic hydrocarbons, molecular gas and atomic gas in NGC 2403

Bendo, G. J.; Wilson, C. D.; Warren, B. E.; Brinks, E.; Butner, H. M.; Chanial, P.; Clements, D. L.; Courteau, Stéphane; Irwin, Judith A.; Israel, F. P.; Knapen, Johan H.; Leech, J.; Matthews, H. E.; Mühle, S.; Petitpas, G.; Serjeant, S.; Tan, Boon-Kok; Tilanus, R. P. J.; Usero, A.; Vaccari, M.; Werf, P. van der; Vlahakis, C.; Wiegert, Theresa; Zhu, Meiping

doi:10.1111/j.1365-2966.2009.16043.x

Cited by 62 publications

(41 citation statements)

References 105 publications

(203 reference statements)

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“…Bendo et al (2010) have used Spitzer imaging of NGC 2403 at 70 μm and 160 μm to map the dust column density via its thermal emission. They also used the far-IR images in conjunction with H i observations to map the gas/dust ratio.…”

Section: An Interstellar Echomentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle¹,

Kotak²,

Farrah³

et al. 2011

ApJ

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We present mid-infrared (MIR) spectroscopy of a Type II-plateau supernova, SN 2004dj, obtained with the Spitzer Space Telescope, spanning 106-1393 days after explosion. MIR photometry plus optical/near-IR observations are also reported. An early-time MIR excess is attributed to emission from non-silicate dust formed within a cool dense shell (CDS). Most of the CDS dust condensed between 50 days and 165 days, reaching a mass of 0.3 × 10 −5 M . Throughout the observations, much of the longer wavelength (>10 μm) part of the continuum is explained as an IR echo from interstellar dust. The MIR excess strengthened at later times. We show that this was due to thermal emission from warm, non-silicate dust formed in the ejecta. Using optical/near-IR line profiles and the MIR continua, we show that the dust was distributed as a disk whose radius appeared to be shrinking slowly. The disk radius may correspond to a grain destruction zone caused by a reverse shock which also heated the dust. The dust-disk lay nearly face-on, had high opacities in the optical/near-IR regions, but remained optically thin in the MIR over much of the period studied. Assuming a uniform dust density, the ejecta dust mass by 996 days was (0.5 ± 0.1) × 10 −4 M and exceeded 10 −4 M by 1393 days. For a dust density rising toward the center the limit is higher. Nevertheless, this study suggests that the amount of freshly synthesized dust in the SN 2004dj ejecta is consistent with that found from previous studies and adds further weight to the claim that such events could not have been major contributors to the cosmic dust budget.

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Section: An Interstellar Echomentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle¹,

Kotak²,

Farrah³

et al. 2011

ApJ

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“…The detailed study of these resolved galaxies will not only act as a benchmark for studies of more distant galaxies, but will also bridge the gap between surveys of distant objects and the extensive Galactic surveys which have superior physical resolution but by their nature are limited to observations of one galaxy. Recent results from the VNGS include determining the nature of dust heating in M81 (Bendo et al 2010), attempting to separate Galactic cirrus emission from extragalactic dust emission in M81 (Davies et al 2010) and studying the dust distribution and heating mechanisms in and around the starburst galaxy, M82 (Panuzzo et al 2010;Roussel et al 2010). While this paper concentrates on the external dust around Cen A, a detailed analysis of the dust within Cen A will be discussed by Parkin et al (2011).…”

Section: Very Nearby Galaxy Surveymentioning

confidence: 99%

“…The data were processed using the MIPS Data Analysis Tools (Gordon et al 2005) along with additional processing steps decribed by Bendo et al (2010) and Bendo et al (in preparation). The additional processing steps include an additional flat-fielding step for the 24-μm data; the removal of latent images from the 24-μm data; background subtraction in all three wave bands (including zodiacal light subtraction in the 24-μm band and short term drift removal in the 70-and 160-μm bands); and a non-linearity correction applied to the 70-μm data.…”

Section: Mid-and Far-infrared Observationsmentioning

confidence: 99%

“…One of the most interesting results to come out of the Spitzer Nearby Galaxy Survey was the tight correlation between the 24-μm emission and the atomic hydrogen spectral line emission from Paschen α, Pα (Calzetti et al 2005(Calzetti et al , 2007Prescott et al 2007;Zhu et al 2008;Kennicutt et al 2009). This suggests that the 24-μm band is a particularly good tracer of star-forming regions (although see Bendo et al 2010 for alternative sources of 24-μm emission). In Fig.…”

Section: Spitzer Imagesmentioning

confidence: 99%

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Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Auld

Smith

Bendo

et al. 2012

Monthly Notices of the Royal Astronomical Society

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International audienceWe present the first results of a multiwavelength survey, incorporating Herschel-, Spitzer, GALEX and Australian Telescope Compact Array (ATCA) observations, of a 1 degrees x 1 degrees field centred on Centaurus A. As well as detecting the inner lobes of the active galactic nucleus (AGN) jet and counterjet, we have found two clouds, bright at submillimetre wavelengths, similar to 15 kpc from the centre of Cen A that are co-aligned with the jets. Flux measurements at Herschel wavelengths have proved vital in constraining fits to the spectral energy distributions (SEDs). The clouds are well fitted by a single-temperature, modified blackbody spectrum (beta= 2) indicating that we are looking at two cold dust clouds on the outskirts of Cen A. The temperature and masses of the clouds are K, K; , and the gas-dust ratio for both clouds is similar to 100. The measured values for the northern dust cloud are consistent with previous measurements from ISO while the southern cloud is a new submillimetre detection. The two dust clouds are located at the termini of the partial H i ring that surrounds Cen A which is also where the gas column density peaks. The Herschel survey encompasses the partial H i ring yet we find no evidence of dust emission in any other part of the ring. Assuming that the gasdust ratio is the same in the rest of the ring, dust mass upper limits in the H i ring are consistent with low column density dust being present but falling below the SPIRE detection limit. We have discussed the origin of these clouds and various possible heating mechanisms. The observations favour a scenario in which the gas and dust were once part of a late-type galaxy, which has since merged with Cen A. The dominant heating mechanism which adequately explains the observed temperatures in both clouds is heating from the evolved stellar population within Cen A

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“…Comparison of the properties of the 8 µm emission and of the CO emission presented in [4] showed that, on large scales, the emission of molecular gas is correlated with the emission of small dust grains, namely, polycyclic aromatic hydrocarbons (PAHs; in particular, their radial profiles have statistically equivalent scale lengths); however, this correlation weakens on smaller scales. Such relationships are interesting because they shed light on the origin of so-called "CO-dark" molecular gas, i.e., gas with a very low CO abundance, even though most of the hydrogen has already been converted into molecular form.…”

Section: Introductionmentioning

confidence: 99%

Relation between the parameters of dust and of molecular and atomic gas in extragalactic star-forming regions

et al. 2017

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The relationships between atomic and molecular hydrogen and dust of various sizes in extragalactic star-forming regions are considered, based on observational data from the Spitzer and Herschel infrared space telescopes, the Very Large Array (atomic hydrogen emission) and IRAM (CO emission). The source sample consists of approximately 300 star-forming regions in 11 nearby galaxies. Aperture photometry has been applied to measure the fluxes in eight infrared bands (3.6, 4.5, 5.8, 8, 24, 70, 100, and 160µm), the atomic hydrogen (21 cm) line and CO (2-1) lines.The parameters of the dust in the starforming regions were determined via syntheticspectra fitting, such as the total dust mass, the fraction of polycyclic aromatic hydrocarbons (PAHs), etc. Comparison of the observed fluxes with the measured parameters shows that the relationships between atomic hydrogen, molecular hydrogen, and dust are different in low-and high-metallicity regions. Low-metallicity regions contain more atomic gas, but less molecular gas and dust, including PAHs. The mass of dust constitutes about 1% of the mass of molecular gas in all regions considered. Fluxes produced by atomic and molecular gas do not correlate with the parameters of the stellar radiation, whereas the dust fluxes grow with increasing mean intensity of stellar radiation and the fraction of enhanced stellar radiation.The ratio of the fluxes at 8 and 24 µm, which characterizes the PAH content, decreases with increasing intensity of the stellar radiation, possibly indicating evolutionary variations of the PAH content. The results confirm that the contribution of the 24 µm emission to the total IR luminosity of extragalactic star-forming regions does not depend on the metallicity. *

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The JCMT Nearby Galaxies Legacy Survey - III. Comparisons of cold dust, polycyclic aromatic hydrocarbons, molecular gas and atomic gas in NGC 2403

Cited by 62 publications

References 105 publications

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Relation between the parameters of dust and of molecular and atomic gas in extragalactic star-forming regions

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