Preliminary spectral observations of the Galaxy with a 7 deg beam by the Cosmic Background Explorer (COBE)

Wright, E. L.; Mather, John C.; Bennett, C. L.; Cheng, E. S.; Shafer, R. A.; Fixsen, D. J.; Eplee, Robert E.; Isaacman, R.; Read, S. M.; Boggess, N. W.; Gulkis, S.; Hauser, M. G.; Janssen, M.; Kelsall, T.; Lubin, P. M.; Meyer, S. S.; Moseley, S. H.; Murdock, T. L.; Silverberg, R. F.; Smoot, G. F.; Weiß, R.; Wilkinson, David T.

doi:10.1086/170641

Cited by 293 publications

(178 citation statements)

References 0 publications

Supporting

Mentioning

162

Contrasting

Order By: Relevance

“…Habart et al (2001) observed efficiencies as high as 3% in the low-UV irradiated Galactic PDR L1721, whereas Vastel et al (2001) also using ISO/LWS fluxes of [C ii] and [O i], found a very low heating efficiency of 0.01% in W49N. The global value for the Milky Way from COBE observations is ∼0.15% (Wright et al 1991). The averages over the entire galaxies observed by e.g.…”

Section: Discussionmentioning

confidence: 98%

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Mookerjea

Krämer

Buchbender

et al. 2011

A&A

View full text Add to dashboard Cite

ContextResults. The [C ii] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [C ii] observed with PACS and CO over the mapped region. There is even less spatial correlation between [C ii] and the atomic gas traced by H i. Detailed comparison of the observed intensities towards the H ii region with models of photo-ionization and photon-dominated regions, confirms that a significant fraction, 20-30%, of the observed [C ii] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio of [C ii] to the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the H ii region.

show abstract

Section: Discussionmentioning

confidence: 98%

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Mookerjea

Krämer

Buchbender

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…It covered the wavelength range from 0.1 to 10 mm in two spectral channels and had approximately 5% spectral resolution and a 7 • field of view (Wright et al 1991;Fixsen et al 1994Fixsen et al , 1997. We extracted a continuum spectrum of the LMC, the SMC being too weak.…”

Section: Firasmentioning

confidence: 99%

Submillimeter to centimeter excess emission from the Magellanic Clouds

Israel¹,

Wall

Raban³

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. Our goal is to determine and study the global emission from the Magellanic Clouds over the full radio to ultraviolet spectral range. Methods. We have selected from the literature those flux densities that include the entire LMC and SMC respectively, and we have complemented these with maps extracted from the WMAP and COBE databases covering the missing 23−90 GHz (13-3.2 mm) and the poorly sampled 1.25-250 THz (240-1.25 μm) spectral ranges in order to reconstruct the global SEDs of the Magellanic Clouds over eight decades in frequency or wavelength. Results. A major result is the discovery of a pronounced excess of emission from the Magellanic Clouds at millimeter and submillimeter wavelengths. We also confirm global mid-infrared (12 μm) emission suppression, and determine accurate thermal radio fluxes and very low global extinctions for both LMC and SMC, the latter being the most extreme in all these respects. Conclusions. These and other dust properties such as the far-UV extinction curve appear to be correlated with (low) metallicity. Possible explanations are briefly considered. As long as the nature of the excess emission is unknown, the total dust masses and gas-to-dust ratios of the Magellanic Clouds cannot reliably be determined

show abstract

“…In Galactic H II regions as well as in the central regions of external galaxies (for instance Howe et al 1991;Stacey et al 1991;Jaffe et al 1994;Malhotra et al 2001;Negishi et al 2001) the luminosity of the [C II] line is typically ∼0.05−0.5% of the far-infrared luminosity (FIR) and correlates well with CO line intensities. For the Milky Way as a whole, the COBE measurements published by Wright et al (1991) correspond to I C II /FIR = 0.1−0.2%. Substantially higher [C II] to far-infrared ratios I [C II] /FIR = 1.6−3.4% occur in high-latitude translucent clouds in the Milky Way (Ingalls et al 2002).…”

Section: Introductionmentioning

confidence: 97%

C⁺emission from the Magellanic Clouds

Israel

Maloney

2011

A&A

View full text Add to dashboard Cite

Context. We study the λ 158 μm [C II] fine-structure line emission from star-forming regions as a function of metallicity. Aims. We have measured and mapped the [C II] emission from the very bright HII region complexes N 11 in the LMC and N 66 in the SMC; as well as the SMC H II regions N 25, N 27, N 83/N 84, and N 88 with the FIFI instrument on the Kuiper Airborne Observatory. Methods. In both LMC and SMC, the ratio of [C II] line to CO line and to the far-infrared continuum emission is much higher than seen almost anywhere else, including Milky Way star-forming regions, and whole galaxies. Results. In the low metallicity, low dust-abundance environment of the LMC and the SMC UV mean free path lengths are much greater than those in the higher-metallicity Milky Way. The increased photoelectric heating efficiencies cause significantly greater relative [C II] line emission strengths. At the same time, similar decreases in PAH abundances have the opposite effect by diminishing photoelectric heating rates. Consequently, in low-metallicity environments relative [C II] strengths are high but exhibit little further dependence on actual metallicity. Relative [C II] strengths are slightly higher in the LMC than in the SMC which has both lower dust and lower PAH abundances.

show abstract

Preliminary spectral observations of the Galaxy with a 7 deg beam by the Cosmic Background Explorer (COBE)

Cited by 293 publications

References 0 publications

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Submillimeter to centimeter excess emission from the Magellanic Clouds

C⁺emission from the Magellanic Clouds

Contact Info

Product

Resources

About

Preliminary spectral observations of the Galaxy with a 7 deg beam by the Cosmic Background Explorer (COBE)

Cited by 293 publications

References 0 publications

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Submillimeter to centimeter excess emission from the Magellanic Clouds

C+emission from the Magellanic Clouds

Contact Info

Product

Resources

About

C⁺emission from the Magellanic Clouds