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Spatially resolved near-infrared spectroscopy of the massive star-forming region IRAS 19410+2336
(EDP SCIENCES S A, 2008-10)
Aims. IRAS 19410+2336 is a young massive star forming region with an intense outflow activity. Outflows are frequently studied in
the near-infrared (NIR) since the H2 emission in this wavelength range often traces the ...
Infrared Spectroscopy of Carbonaceous-chondrite Inclusions in the Kapoeta Meteorite: Discovery of Nanodiamonds with New Spectral Features and Astrophysical Implications
(IOP Publishing, 2018-03-22)
We report the finding of nanodiamonds, coexisting with amorphous carbon, in carbonaceous-chondrite (CC) material from the Kapoeta achondritic meteorite by Fourier-transform infrared (FTIR) spectroscopy and micro-Raman ...
High-resolution radio study of SNR IC443 at low radio frequencies
(EDP Sciences, 2011-04)
Aims. We investigate the morphology at low radio frequencies of the supernova remnant (SNR) IC 443 in detail and accurately establish its radio continuum spectral properties. Methods. We used the VLA in multiple configurations ...
The earliest phases of high mass star formation, as seen in NGC 6334 by Herschel HOBYS
(EDP Sciences, 2017)
Aims. To constrain models of high-mass star formation, the Herschel-HOBYS key program aims at discovering massive dense cores (MDCs) able to host the high-mass analogs of low-mass prestellar cores, which have been searched ...
The dust properties and physical conditions of the interstellar medium in the LMC massive star-forming complex N11
(OXFORD UNIV PRESS, 2016)
We combine Spitzer and Herschel data of the star-forming region N11 in the Large Magellanic Cloud (LMC) to produce detailed maps of the dust properties in the complex and study their variations with the interstellar-medium ...
Multifrequency study of HH 137 and HH 138: Discovering new knots and molecular outflows with Gemini and APEX
(Wiley Blackwell Publishing, Inc, 2020-08)
We present a multiwavelength study of two Herbig-Haro (HH) objects (137 and 138) that may be associated. We use Gemini H2 (2.12 μm) and K (2.2 μm) images, as well as Atacama Pathfinder EXperiment molecular line observations ...