Search Results - (Author, Cooperation:G. Anglada)
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1Latest Papers from Table of Contents or Articles in PressC. Carrasco-Gonzalez ; J. M. Torrelles ; J. Canto ; S. Curiel ; G. Surcis ; W. H. Vlemmings ; H. J. van Langevelde ; C. Goddi ; G. Anglada ; S. W. Kim ; J. S. Kim ; J. F. Gomez
American Association for the Advancement of Science (AAAS)
Published 2015Staff ViewPublication Date: 2015-04-04Publisher: American Association for the Advancement of Science (AAAS)Print ISSN: 0036-8075Electronic ISSN: 1095-9203Topics: BiologyChemistry and PharmacologyComputer ScienceMedicineNatural Sciences in GeneralPhysicsPublished by: -
2Latest Papers from Table of Contents or Articles in PressG. Anglada-Escude ; M. Tuomi
American Association for the Advancement of Science (AAAS)
Published 2015Staff ViewPublication Date: 2015-03-07Publisher: American Association for the Advancement of Science (AAAS)Print ISSN: 0036-8075Electronic ISSN: 1095-9203Topics: BiologyChemistry and PharmacologyComputer ScienceMedicineNatural Sciences in GeneralPhysicsPublished by: -
3Articles: DFG German National LicensesGómez, Y. ; Anglada, G. ; Torrelles, J. M. ; Miranda, L. F.
[s.l.] : Macmillian Magazines Ltd.
Published 2001Staff ViewISSN: 1476-4687Source: Nature Archives 1869 - 2009Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsNotes: [Auszug] A star like the Sun becomes a planetary nebula towards the end of its life, when the envelope ejected during the earlier giant phase becomes photoionized as the surface of the remnant star reaches a temperature of ∼30,000 K. The spherical symmetry of the giant phase is lost in the ...Type of Medium: Electronic ResourceURL: -
4Articles: DFG German National LicensesTorrelles, J. M. ; Patel, N. A. ; Gómez, J. F. ; Rodríguez, L. F. ; Anglada, G. ; Garay, G. ; Greenhill, L. ; Curiel, S. ; Cantó, J. ; Ho, P. T. P.
[s.l.] : Macmillian Magazines Ltd.
Published 2001Staff ViewISSN: 1476-4687Source: Nature Archives 1869 - 2009Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsNotes: [Auszug] The exact processes by which interstellar matter condenses to form young stars are of great interest, in part because they bear on the formation of planets like our own from the material that fails to become part of the star. Theoretical models suggest that ejection of gas during early phases ...Type of Medium: Electronic ResourceURL: -
5Articles: DFG German National LicensesStaff View
ISSN: 1572-946XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract Maps of the CS (J=1→0) emission at 49 GHz of L43 (RNO 91), NGC 2068 (HH 19-27) and L1524 (Haro 6-10) are presented. Physical parameters of these clouds are derived from the observations. The CS emission is compared with ammonia emission maps obtained with a similar angular resolution. Both CS and ammonia molecules are tracers of the high-density gas in molecular clouds. Thus, a similar distribution of the emission is expected. However, our observations show evidence of some remarkable morphological differences.Type of Medium: Electronic ResourceURL: -
6Articles: DFG German National LicensesLópez, R. ; Morata, O. ; Sepúlveda, I. ; Estalella, R. ; Anglada, G. ; Pastor, J. ; Planesas, P.
Springer
Published 1994Staff ViewISSN: 1572-946XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract We present CS(J = 1 → 0) observations of the high density gas in a sample of eleven star forming regions with molecular or optical outflows. The sources of this sample cover a wide range of physical sizes. All these sources had been previously mapped in NH3 (1,1) with similar angular resolution. In all the sources of this sample CS emission was detected, indicating a global correlation between the emissions traced by the CS and the NH3 molecules. However, the detailed characteristics of these two emissions (e.g., the extent and the location of the emission peak) show, in general, significant differences in the sources which are well resolved by the beam. As a general trend, the emission traced by the NH3 molecule appears as compact clumps which engulf an outflow activity center. In contrast, the emission traced by the CS molecule, usually more extended, appears as a background which connects different outflow activity centers associated with each NH3 clump.Type of Medium: Electronic ResourceURL: -
7Articles: DFG German National LicensesStaff View
ISSN: 1572-946XKeywords: HH objects: individual: HH 30, HH 262Source: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract New, deep, wide-field [SII] images of the HL Tauri region show the extended spatial structure of the HH 30 jet and counter-jet. At an angular distance of ∼ 300 arcsec toward the NE, the HH 30 jet ends in a group of scattered condensations. This previously undetected structure might correspond to a broken-up working surface. Our images also include HH 262, which is shown to have a previously undetected extended emission region.Type of Medium: Electronic ResourceURL: -
8Articles: DFG German National LicensesVerdes-Montenegro, L. ; Torrelles, J. M. ; Rodriguez, L. F. ; Anglada, G. ; Lopez, R. ; Estallella, R. ; Canto, J. ; Ho, P. T. P.
Springer
Published 1990Staff ViewISSN: 1572-946XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract The (J, K)=(1,1) ammonia transition emission has been observed toward six regions with signs of active star formation (AFGL 5142, HH 33/40, AFGL 5157, AFGL 6366S, HHL 73, and S140N), using the 37 m antenna of the Haystack Observatory. We detected and mapped the ammonia emission in all of these sources with the exception of HH 33/40. The (J, K)-(2,2), ammonia transition was also observed at the peak position of each source in order to obtain the rotational temperature of the ammonia clumps.Type of Medium: Electronic ResourceURL: