[PDF] Top 20 Water in low-mass star-forming regions with Herschel
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Water in low-mass star-forming regions with Herschel
... K), water is predominantly found on dust grains in the form of water ...form water ice ...2010). Water vapour can form in the gas phase through ion-molecule chemistry at low ... See full document
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Punanova, Anna (2017): Chemistry and kinematics in low-mass star-forming regions. Dissertation, LMU München: Fakultät für Physik
... various regions (in particular the amount of external illumination, gas volume density ...same regions, we do not notice any trend, which may be caused by dust temperatures (mainly derived from ... See full document
167
Ultracool dwarfs in open clusters and star-forming regions
... and mass functions using the NextGen and DUSTY models from the Lyon group for consistency [31, ...to low-mass stars and brown dwarfs. The mass functions for Per, the Pleiades, and Praesepe are ... See full document
7
Spitzer catalog of Herschel selected ultrared dusty, star forming galaxies
... end of our sample. Since leaving redshift as a free pa- rameter introduces extra degree of freedom and degen- eracy in SED fitting than fixing the redshift, here we also compare with the magphys results by fixing the in- ... See full document
33
Looking deep into the Rosette Nebula's heart : the (sub)stellar content of the massive young cluster NGC 2244
... between low-mass stars and BDs is typically found in the range 2 – ...the star-to-BD ratio ( uncertainties in distances, ages, use of different evolutionary models, reddening laws, membership issues, ... See full document
22
Comparisons between different techniques for measuring mass segregation
... observed star-forming regions display a range of fractal dimensions (Cartwright & Whitworth 2004; Schmeja et ...all regions may form with the same (low) fractal dimension, and ob- ... See full document
14
Testing the universality of star formation - II. Comparing separation distributions of nearby star-forming regions and the field
... et al. 1999). Due to the dispersion of this cluster, searches for mem- bers are incomplete, but > 100 high-mass members have been iden- tified through their proper motion and parallaxes (de Zeeuw et al. 1999) ... See full document
11
Fragmentation and disk formation during high-mass star formation. IRAM NOEMA (Northern Extended Millimeter Array) large program CORE
... lower mass fragments close to the global Jeans mass were not detected in these ...lower mass fragments (Zhang et ...less-evolved regions such as those in Wang et ...of low-mass ... See full document
28
Methods and Results Toward Measuring Magnetic Fields in Star-Forming Regions
... of star formation and evolution, and the cycle of insterstellar material, including dust grains and ...the star formation process (Mouschovias 2001), especially in the low-mass ... See full document
142
The evolution of post starburst galaxies from z=2 to 0 5
... different regions of super-colour ...recent star formation (quiescent galaxies) form a tight and well-defined ‘red sequence’ with low ...The star-forming population of galaxies covers a ... See full document
13
Testing the universality of star formation - I. Multiplicity in nearby star-forming regions
... primary mass (Duquennoy & Mayor 1991; Fischer & Marcy 1992; Lada ...primary mass (at least from M dwarfs to G dwarfs), and so this mass dependence may reflect a primordial ... See full document
18
Weak and compact radio emission in early high mass star forming regions II The nature of the radio sources
... In Rosero et al. ( 2016, hereafter Paper I ) we described our high-sensitivity (∼ 3 – 10 μ Jy beam − 1 ) continuum survey, which aimed to identify candidates in early evolutionary phases of high-mass star ... See full document
23
Modelling high resolution ALMA observations of strongly lensed highly star forming galaxies detected by Herschel
... the Herschel Space Observatory. Our modelling recovers mass properties of the lensing galaxies and, by determining magnification factors, in- trinsic properties of the lensed sub-millimetre ...of ... See full document
13
Spitzer IRAC Colors of Nebulae Associated with Star Forming Regions
... II regions, W5-East (W5-E) and W5-West. The ionizing star in W5-E is an O7V star, BD +59˚ ...of low-mass stars in this ...small regions to investigate the nebular color (Figure ... See full document
12
A network of filaments detected by Herschel in the Serpens core : a laboratory to test simulations of low mass star formation
... new Herschel maps of Serpens presented in this paper are dominated by what is known as the Serpens core cluster and also by the complex around a group of four T Tauri stars, called G3 to G6 (see ...Be star ... See full document
16
Disk Outflow Models as Applied to High Mass Star Forming Regions through Methanol and Water Maser Observations
... sources, lending further support to theoretical models that predict methanol masers are pumped by infrared dust emission in the vicinity of high-mass protostars. [17] observed 44 GHz Class I and 6.7 GHz Class II ... See full document
28
1-10 Myr-old Low Mass Stars and Brown Dwarfs in Nearby Star Forming Regions
... extremely low mass objects may not follow the same path as that for their higher mass stellar ...high mass disk destruction requires a high flux of EUV Lyman continuum photons from a hot ... See full document
222
1-10 Myr-old low mass stars and brown dwarfs in nearby star forming regions
... I have studied the h and χ “double cluster” using modern imaging and spectroscopic techniques. My conclusions differ with those of previous studies such as Wildey’s (1964) largely due to my recognition of the significant ... See full document
12
Alfvén waves in low mass star forming regions
... a low-mass sta r-forming region: the cooling of a num ber of molecular species and ionized carbon, tog ethe r with the heating due to cosmic rays and the Alfvén waves suppor ting the ...central ... See full document
178
The JCMT Gould Belt Survey : low mass protoplanetary discs from a SCUBA 2 census of NGC 1333
... Table 1. NGC 1333 protoplanetary disc candidates; note that object #59 is blended with #58 (Fig. 1), so it is uncertain which source dominates the emission. Object #59 is located in the pixel of the peak emission, while ... See full document
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