Physical Structure of Planetary Nebulae. II. NGC 7662

2004 ◽  
Vol 128 (4) ◽  
pp. 1705-1710 ◽  
Author(s):  
Martín A. Guerrero ◽  
Elizabeth G. Jaxon ◽  
You-Hua Chu
Keyword(s):  
Planetary Nebulae ◽  
Physical Structure ◽  
Ngc 7662

Physical Structure of Planetary Nebulae. I. The Owl Nebula

2003 ◽  
Vol 125 (6) ◽  
pp. 3213-3221 ◽  
Author(s):  
Martn A. Guerrero ◽  
You-Hua Chu ◽  
Arturo Manchado ◽  
Karen B. Kwitter
Keyword(s):  
Planetary Nebulae ◽  
Physical Structure

scholarly journals Physical Structure of Planetary Nebulae. III. The Large and Evolved NGC 1360

2004 ◽  
Vol 128 (4) ◽  
pp. 1711-1715 ◽  
Author(s):  
Daniel B. Goldman ◽  
Martín A. Guerrero ◽  
You-Hua Chu ◽  
Robert A. Gruendl
Keyword(s):  
Planetary Nebulae ◽  
Physical Structure

scholarly journals Ultraviolet spectra of planetary nebulae - VI. NGC 7662

1982 ◽  
Vol 199 (3) ◽  
pp. 517-564 ◽  
Author(s):  
J. P. Harrington ◽  
M. J. Seaton ◽  
S. Adams ◽  
J. H. Lutz
Keyword(s):  
Planetary Nebulae ◽  
Ultraviolet Spectra ◽  
Ngc 7662

High dispersion spectra of Planetary Nebulae

1997 ◽  
Vol 180 ◽  
pp. 242-242
Author(s):  
S. Hyung ◽  
L. H. Aller
Keyword(s):  
Plasma Diagnostics ◽  
Surface Brightness ◽  
High Surface ◽  
Planetary Nebulae ◽  
High Dispersion ◽  
Chemical Compositions ◽  
Echelle Spectrograph ◽  
High Surface Brightness ◽  
Low Surface Brightness ◽  
Ngc 7662

Determinations of the plasma diagnostics and chemical compositions of planetary nebulae require ultimately high dispersion spectra. For objects of high surface brightness the Hamilton Echelle Spectrograph at Lick Observatory is satisfactory for the region 3650–10100Å which involves the 168th to 56th echelle orders. For a slit width of 640 μm amounting to 1.15 arcsec at the Coude focus, the actual spectral resolution (FWHM) is about 0.2Å at 8850Å. The length of the slit is chosen as 4.0 arcsec. Hyung (1994) & Aller (1994) describe the observing procedure. Since the Hamilton echelle was designed primarily for star-like sources, it is not useful for extended low surface brightness PN. The earlier observations were obtained with an 800 × 800 chip that did not cover the echelle field, so several settings were needed. Later, we used a slower 2048 × 2048 chip which covered the whole field and was somewhat more efficient at longer wavelengths. The program has been completed and definitive measurements have obtained for NGC 2440, NGC 6543, NGC 6741, NGC 6818, NGC 7026, NGC 7662, and Hu 1-2. All of these PN display particularly rich, interesting spectra. Previously observed and published objects include IC 351, IC 418, IC 2149, IC 4997, NGC 6567, NGC 6572, NGC 6790, NGC 6886, NGC 7009, BD +30 3639, & Hubble 12. NGC 6884 is in press. Additional nebulae which are yet to be discussed are IC 4634, IC 4846, IC 5117, NGC 6210, & NGC 6803.

scholarly journals The physical structure of planetary nebulae around sdO stars: Abell 36, DeHt 2, and RWT 152★

2014 ◽  
Vol 446 (1) ◽  
pp. 317-329 ◽  
Author(s):  
A. Aller ◽  
L. F. Miranda ◽  
L. Olguín ◽  
R. Vázquez ◽  
P. F. Guillén ◽  
...  
Keyword(s):  
Planetary Nebulae ◽  
Physical Structure

scholarly journals High-Resolution Spectroscopy of the Planetary Nebulae PM 1–242, PM 1–318 and PM 1–322

2010 ◽  
Vol 27 (2) ◽  
pp. 199-202 ◽  
Author(s):  
L. F. Miranda ◽  
R. Vázquez ◽  
M. A. Guerrero ◽  
C. B. Pereira ◽  
E. Iñiguez-Garín
Keyword(s):  
High Resolution ◽  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Central Star ◽  
Brightness Distribution ◽  
Physical Structure ◽  
High Resolution Spectroscopy

AbstractWe have recently confirmed the planetary nebula (PN) nature of PM 1–242, PM 1–318 and PM 1–322. Here we present high-resolution long-slit spectra of these three PNe in order to analyze their internal kinematics and to investigate their physical structure. PM 1–242 is a tilted ring and not an elliptical PN as suggested by direct images. The object is probably related to ring-like PNe and shows an unusual pointsymmetric brightness distribution in the ring. PM 1–318 is a pole-on elliptical PN, instead of a circular one as suggested by direct images. PM 1–322 is spatially unresolved and its spectrum shows large differences between the forbidden lines and Hα profiles, with the latter showing a double-peaked profile and relatively extended wings (FWZI ~325 km s−1). These properties are found in other PNe that are suspected to host a symbiotic central star.

scholarly journals On the relationship between the H2 emission and the physical structure of planetary nebulae

2012 ◽  
Vol 429 (2) ◽  
pp. 973-986 ◽  
Author(s):  
R. A. Marquez-Lugo ◽  
G. Ramos-Larios ◽  
M. A. Guerrero ◽  
R. Vázquez
Keyword(s):  
Planetary Nebulae ◽  
Physical Structure ◽  
The Relationship
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