منابع مشابه
Water maser emission in IC 342
The detection of 22GHz water vapor emission from IC 342 is reported, raising the detection rate among northern galaxies with IRAS point source fluxes S100μm > 50 Jy to 16%. The maser, associated with a star forming region ∼10–15 west of the nucleus, consists of a single 0.5 kms wide feature and reaches an isotropic luminosity of 10 L⊙ (D=1.8Mpc). If the time variability is intrinsic, the maser ...
متن کاملSearch for 183 GHz water maser emission in starburst galaxies
We have searched for water vapor emission at 183 GHz, redshifted at 157 GHz and 161 GHz, in the two ultraluminous starburst galaxies Mkn 1014 and VIIZw244. Due to the low energy level of the upper state of the 183 GHz transition (≈ 200K), it is expected that the emission regions are extended, as they are in the Orion or W49Nmolecular cloud cores. Since the warm and dense gas, typical of star-fo...
متن کاملMaser emission in planetary nebulae
Stars at the top of the asymptotic giant branch (AGB) can exhibit maser emission from molecules like SiO, H2O and OH. These masers appear in general stratified in the envelope, with the SiO masers close to the central star and the OH masers farther out in the envelope. As the star evolves to the planetary nebula (PN) phase, mass-loss stops and ionization of the envelope begins, making the maser...
متن کاملExtragalactic water masers in bright IRAS sources
We report the results of a search for 22GHz water maser emission in IRAS-bright galaxies, using the 100-m Effelsberg telescope. In particular, we present the details of four new maser detections (IC 342, NGC 2146, NGC 3556, and Arp 299) and follow-up interferometric studies. A comparison between water maser detection rates derived in the present study and those in previous similar surveys is al...
متن کاملVla Observations of Water Maser Emission Associated with Svs 13 and Other Sources in Ngc 1333
The young stellar object SVS 13 is believed to power the chain formed by the HH 7-11 objects. Recent observations have revealed that in the radio continuum (3.6-cm) the source is a binary with components separated by about 0. 00 3 in the east-west direction. The members of the binary are named VLA 4A (western component) and VLA 4B (eastern component). In an attempt to ascertain which of the two...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2002
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20020199