Far-IR selected star formation regions
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Far-IR selected star formation regions

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Published by National Aeronautics and Space Administration, Ames Research Center in Moffett Field, Calif .
Written in English

Subjects:

  • Infrared technology,
  • Interstellar matter

Book details:

Edition Notes

Other titlesFar-I.R. selected star formation regions
StatementD.T. Jaffe ... [et al.]
SeriesNASA technical memorandum -- 85955
ContributionsJaffe, D. T, Ames Research Center
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL14926483M

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Detailed far-IR observations and complementary submillimeter, 5 GHz continuum and C(O) observations of a sample of eight far-IR selected luminous regions of star formation are presented. The far infrared (far-IR) can be an important spec-tral region for material analysis. Applications include studies of lattice vibrations in crystals, anti-ferromagnetic resonance and energy gap measurements in superconductors. 1 Conventional methods for sample analysis for the far-IR spectral region include the preparation of a fi lm, a mull or a. The Star Formation Reference Survey Goals By having both a statistical sample of galaxies and a complete sampling of the SEDs from the X-ray/UV to the far-IR and radio,allows us to: a) cross-calibrate the majority of star-formation rate indicators in different types of galaxies (e.g. Fig 3). The far-IR continuum The use of the far-IR emission from warm dust associated with the star formation region may provide a more reliable estimate of the SFR [31, 40].However, star formation rates derived in this way most frequently assume that the dust is effectively acting as a re-processing bolometer wrapped around the star forming region, and that cool and old stars do not provide too much.

The lack of observations of the earliest stages in high-mass star formation motivated the selection of massive star-forming regions using the µm ISOPHOT Serendipity : Martin Hennemann. To understand star formation, we have to study the conditions necessary for interstellar clouds to contract. Consider for simplicity a spherical homogeneous cloud of mass M, radius R, temperature T, and density ρ (see Figure ). The easiest way to test if such a cloud is stable or contracting is by testing the virial equilibrium. The most common approach for measuring SFRs in resolved regions, such as regions within the Milky Way, is to count individual objects or events (e.g., supernovae) that trace the recent star formation (Chomiuk & Povich ). In the molecular clouds within kpc of the solar system, this is accomplished by counting young stellar objects. Abstract. In this paper, we present a sample of cluster galaxies devoted to study the environmental influence on the star formation activity. This sample of galaxies inhabits in clusters showing a rich variety in their characteristics and have been observed by the SDSS-DR6 down to M{sub B} {approx} , and by the Galaxy Evolution Explorer AIS throughout sky regions corresponding to several.

Herschel-PACS spectra covering um are analyzed for ten high-mass star forming regions of various luminosities and evolutionary stages at spatial scales of ~10^4 AU. Radiative transfer models are used to determine the contribution of the envelope to the far-IR CO by: far-IR ~ 3 × /µ L Cloverleaf quasar: z = , L far-IR ~ 6 × /µ L Line is bright: to % of the far-IR continuum Optically thin, high n, high T limit ⇒ Calculate minimum mass of ionized gas: 2 to 16% of molecular ISM Values range from few to 20% (M82, Lord et al. ) in star forming galaxies. The Astro Science Frontiers Panel on Planetary Systems and Star Formation was charged to consider science opportunities in the domain of planetary systems and star formation—including the perspectives of astrochemistry and exobiology—spanning studies of molecular clouds, protoplanetary and debris disks, and extrasolar planets, and the. star formation." In addition a new hypothesis is advocated on the two modes of star formation associated with HII regions, i.e., the cluster and dispersed modes. The former gives birth to a rich cluster and in the associated HII region BRCs are formed only at a later stage of its evolution in the peripheries.