Szó szerinti fordításban az impostor=csaló. Magyar elnevezesevel, magyarításával én még nem találkoztam. Ha lehet javasolni valamit, én a csalót kihúznám a listáról (nem szép), inkább valami más kellene (pl. szupernóva-kinézetű? Szupernóva-imitátor? (Bár ebben semmi sem magyar.) Álszupernóva? Talán ez a legjobb eddig.) Sz.
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Von: mira-bounces@mcse.hu [mira-bounces@mcse.hu]" im Auftrag von "FIDRICH Robert [fidusz@zpok.hu]
Gesendet: Dienstag, 18. Januar 2011 17:48
Bis: mira@mcse.hu
Betreff: [Mira] mijaza "supernova impostor"? - PSN J10523453+2256052 IN NGC 3437
Sziasztok!
A CBET 2637 szerint az NGC 3437-ben a CTRS csapat talált egy
szupernóvát. Azt írja a CBET hogy Vinkó Józsiék szerint ez az objektum valójában egy
"supernova impostor".
Kérdéseim:
1) Mi a magyar elnevezések ezeknek a "szupernóva imposztoroknak"?
2) A Wikipédia szerint "One supernova impostor that made news after the
fact was the one observed on October 20, 2004, in the galaxy UGC 4904 by
Japanese amateur astronomer Koichi Itagaki. This LBV star blew itself up
just two years later, on October 11, 2006, as supernova SN 2006jc."
Lehet, hogy ebből a csillagból is rendes szupernóva lesz pár éven belül?
* * *
PSN J10523453+2256052 IN NGC 3437
S. Howerton, Arkansas City, KS, U.S.A.; A. J. Drake, S. G. Djorgovski, A.
Mahabal, M. J. Graham, and R. Williams, California Institute of Technology;
J. L. Prieto, Carnegie Observatories; M. Catelan, Pontificia Universidad
Catolica de Chile; E. C. Beshore and S. M. Larson, Lunar and Planetary
Laboratory, University of Arizona; and E. Christensen, Gemini Observatory,
reported (on Jan. 12) the Catalina Real-time Transient Survey´s discovery
of an apparent supernova in public images from the Catalina Sky Survey (CSS).
The object is located at R.A. = 10h52m34s.53, Decl. = +22d56´05".2 (equinox
2000.0), which is 16".9 west and 2".2 north of the center of NGC 3437 (which
itself has redshift z = 0.0042). CSS unfiltered-CCD magnitudes for the new
object, which was designated PSN J10523453+2256052 and posted on the Central
Bureau´s "Transient Objects Confirmation Page": 2010 Dec. 11.47 UT, [19.5;
2011 Jan. 3.45, 19.1; 10.41, 18.4 (discovery observation). The type-Ic
supernova 2004bm had position end figures 35s.33, 05".5 (cf. IAUC 8335).
J. Vinko, University of Szeged; J. C. Wheeler and E. Chatzopoulos,
University of Texas; and G. H. Marion, Harvard-Smithsonian Center for
Astrophysics and University of Texas, report that PSN J10523453+2256052
appears to be a "supernova impostor" similar to SN 2008S (Smith et al.
2009, Ap.J. 697, L49; Botticella et al. 2009, MNRAS 398, 1041). A spectrum
obtained on 2011 Jan. 15.30 UT with the 9.2-m Hobby-Eberly Telescope (+
Marcario Low-Resolution Spectrograph, range 420-1020 nm) by J. Caldwell shows
prominent, narrow Balmer emission lines superimposed on a blue continuum. No
other spectral features are detected. The absence of Na D absorption and the
presence of the blue continuum argues against significant reddening. Unlike
SN 2008S, the Ca II infrared triplet is not detected in PSN J10523453+2256052.
The FWHM of H-alpha is about 1000 km/s. The redshift estimated from the
emission peaks is z = 0.0047, in agreement with that of the host galaxy, NGC
3437. At the mean distance of 25 Mpc listed in NED, the absolute magnitude
would be -13.6, which is consistent with the brightness of supernova impostors
and much less bright than normal supernovae.
S. Taubenberger, Max-Planck-Institut fuer Astrophysik; A. Pastorello,
Queen´s University; N. Elias-Rosa, Institute for Space Studies, Institut de
Ciencies de l´Espai, IEEC, Consejo Superior de Investigaciones Cientificas;
S. Benetti, Istituto Nazionale di Astrofisica (INAF), Padova; and F. Bufano,
INAF, Catania, on behalf of a larger collaboration, report that a spectrogram
(range 380-960 nm, resolution 1.2 nm) of PSN J10523453+2256052 was obtained
with the 2.2-m telescope (+ CAFOS) of the Calar Alto Observatory on Jan. 17.1
UT. The spectrum shows a rather flat continuum with prominent and narrow
(FWHM about 1200 km/s) hydrogen lines in emission; weak Fe II lines are also
detected. The spectral characteristics and the faint absolute magnitude at
discovery resemble those expected in the eruption of a luminous blue variable.
A follow-up campaign for this transient is in progress.
--
Fidusz (FIDRICH Robert)
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