scholarly journals NIR Fabry-Perot Imaging Spectroscopy of PNe

2003 ◽  
Vol 209 ◽  
pp. 257-258
Author(s):  
Lorena Arias ◽  
Margarita Rosado
Keyword(s):  
Velocity Field ◽  
Radial Velocity ◽  
Molecular Hydrogen ◽  
Near Infrared ◽  
Imaging Spectroscopy ◽  
Planetary Nebulae ◽  
Physical Parameters ◽  
Excitation Mechanism ◽  
Vibrationally Excited ◽  
Fabry Perot

In this work we report the radial velocity field of the molecular hydrogen in five planetary nebulae, obtained from scanning Fabry-Perot interferometer observatins at the near-infrared vibrationally excited line H2 S(1) 1-0 at 2.122 μm. Direct images of the nebulae in both transitions of molecular hydrogen S(1) 1-0 and S(1) 2-1 are used in order to discriminate between shocks and fluorescence as the excitation mechanism of the H2. Finally, some physical parameters are derived.

scholarly journals Fabry-Pérot Radial Velocities of S274: a Planetary Nebula

1983 ◽  
Vol 103 ◽  
pp. 547-547
Author(s):  
E. Recillas-Cruz ◽  
P. Pismis
Keyword(s):  
Velocity Field ◽  
Radial Velocity ◽  
Planetary Nebula ◽  
Outer Boundary ◽  
Radial Velocities ◽  
Physical Parameters ◽  
Expansion Velocity ◽  
Double Points ◽  
Fabry Perot ◽  
The Mean

The bright nebula S274 (YM29), 8′ across has been classified as a planetary by Abell (1966) although it has been considered a SNR by other authors. We have determined radial velocities at 173 points on this nebula from four Fabry-Pérot interferograms. The velocity field exhibits a great deal of structure. The average expansion velocity is + 31.5 ± 8 km s−1. The mean radial velocity of S274 is not well determined due to the nature of the velocity field, while the overall velocity (173 points) is + 33 ± 21 km s−1. Points at the outer boundary yield an average of 22 ± 14 km s−1 while the average of the double points is 25 km s−1. The age of expansion of the nebula is estimated at 6.8 × 103yr. The physical parameters of this object are consistent with those of a planetary nebula.

scholarly journals Near–Infrared Imaging of Proto-Planetary Nebulae

1993 ◽  
Vol 155 ◽  
pp. 340-340 ◽  
Author(s):  
R.E.S. Clegg ◽  
N. A. Walton ◽  
M.J. Barlow
Keyword(s):  
Molecular Hydrogen ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Planetary Nebulae ◽  
Agb Stars ◽  
Intermediate Mass ◽  
Preliminary Results ◽  
Near Ir ◽  
Intermediate Mass Stars ◽  
Hydrogen Lines

It is not really known how low and intermediate mass stars eject mass to form PNs. We present preliminary results from a programme of near–IR imaging, in which we study a sequence of objects, from extreme AGB stars through proto–planetaries to young, compact PNs. We aim to study the sequence of morphologies, to see where the onset of bipolar shaping occurs, and to use the IR molecular hydrogen lines to map neutral regions around ionized nebulae.

A near-infrared fabry-perot imager at CRL 1.5m telescope and the structure and velocity field of shocked H2 emission in orion KL region

1994 ◽  
Vol 3 (1-4) ◽  
pp. 315-316
Author(s):  
H. Sugai ◽  
T. Usuda ◽  
H. Kawabata ◽  
M. Y. Inoue ◽  
H. Kataza ◽  
...  
Keyword(s):  
Velocity Field ◽  
Near Infrared ◽  
Fabry Perot

scholarly journals Investigating the near-IR properties of PN: Deep imaging of molecular hydrogen emission

1997 ◽  
Vol 180 ◽  
pp. 254-254
Author(s):  
William B. Latter ◽  
Joseph L. Hora
Keyword(s):  
Planetary Nebula ◽  
Near Infrared ◽  
Morphological Evolution ◽  
Imaging Study ◽  
Planetary Nebulae ◽  
Central Star ◽  
Circumstellar Envelope ◽  
Excitation Mechanism ◽  
Imaging Data ◽  
Uv Photons

We present the first results of a deep near-infrared narrowband imaging study of several planetary nebulae. The data were acquired using the University of Hawaii 2.2m telescope on Mauna Kea and the “QUIRC” 1024 × 1024 array camera. With these sensitive high spatial resolution imaging data, we are able to explore in detail where H2 is found relative to the ionized region in planetary nebulae at various stages of evolution (See Figure 1, for an example). The objects were selected from previous studies to have evidence for extended emission from H2, and they are at several differing phases of central star evolution. The presence of molecules in the UV–flooded environment of a planetary nebula cannot be explained without highly non-spherical geometries and high densities, or clumping. Although there can be an ambiguity in the excitation mechanism (UV photons or shocks), the location of H2 emission identifies regions of the nebula with sufficient dust shielding and density for the survival of molecular species. The emission morphology also provides information that helps identify which excitation mechanism is most likely. When combined with data provided by other molecular studies, we can examine how the photodissociation region evolves through the circumstellar envelope as the planetary nebula tracks across the top of the HR diagram. We can also consider how morphological evolution of the nebula, through interacting winds and shocks, might provide the conditions necessary for molecular survival.

IR Fabry-Perot imaging of NGC 3132

1997 ◽  
Vol 180 ◽  
pp. 205-205
Author(s):  
L. E. Allen ◽  
M.C.B. Ashley ◽  
S. D. Ryder ◽  
J.W.V. Storey ◽  
Y-S. Sun ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Near Infrared ◽  
New South ◽  
New South Wales ◽  
Planetary Nebulae ◽  
Emission Lines ◽  
South Wales ◽  
Fabry Perot

Near-infrared (1-3μm) emission lines of molecular and ionized hydrogen are excellent tools for investigating the morphology, energetics and kinematics of planetary nebulae, especially those PNe which contain large amounts of dust and are thus obscured at shorter wavelengths. The southern planetary nebula NGC 3132 was imaged with UNSWIRF (University of New South Wales Infrared Fabry-Perot) and IRIS on the 3.9m AAT Images in the H2 v=1-0 S(1) and H2 v=2-1 S(1) lines at 2.12μm and 2.25μm, and in Hii Brγ at 2.16μm are presented.

scholarly journals 2D kinematics of the edge-on spiral galaxy ESO 379-006

2012 ◽  
Vol 8 (S295) ◽  
pp. 234-235
Author(s):  
M. Rosado ◽  
R. F. Gabbasov ◽  
P. Repetto ◽  
I. Fuentes-Carrera ◽  
P. Amram ◽  
...  
Keyword(s):  
Velocity Field ◽  
Radial Velocity ◽  
Rotation Curve ◽  
Minor Axis ◽  
Ionized Gas ◽  
Diffuse Ionized Gas ◽  
Fabry Perot ◽  
The Galaxy ◽  
Rotation Motion

AbstractWe present a kinematical study of the marginally edge-on galaxy ESO 379-006. With Fabry-Perot spectroscopy at Hα we obtain velocity maps, the radial velocity field, and position-velocity diagrams parallel to the major and to the minor axis of the galaxy. We build the rotation curve of the galaxy and discuss the role of projection effects. The twisting of isovelocities in the radial velocity field of the disk of ESO 379-006 as well as a kinematical asymmetry found in the position-velocity diagrams parallel to the minor axis suggest the existence of non-circular motions that can be modeled by including a radial inflow besides the rotation motion. Extraplanar Diffuse Ionized gas was detected in this galaxy both from the images and from its kinematics. It is possible that the diffuse gas is lagging in rotation.

scholarly journals Millimeter-Wave Observations of Planetary Nebulae

1978 ◽  
Vol 76 ◽  
pp. 328-328
Author(s):  
Hugh M. Johnson
Keyword(s):  
Spectral Index ◽  
Millimeter Wave ◽  
Research Program ◽  
Near Infrared ◽  
Journal Article ◽  
Planetary Nebulae ◽  
Astronomy Observatory ◽  
Independent Research ◽  
Fabry Perot ◽  
Infrared Data

Observations of the integrated continuum flux density of several stellar planetary nebulae have been made at 90 GHz. These are reported, with some remarks on their significance for objects with positive radio-frequency spectral index, and to display graphically their relation to published microwave and near-infrared data. The 90-GHz data have been obtained with the 11-m dish of the National Radio Astronomy Observatory* on Kitt Peak, under the Lockheed Independent Research Program. Three of the objects have been included among a dozen stellar planetary nebulae observed with the Fabry-Perrot interferometer at the Cerro Tololo Inter-American Observatoryt so as to provide kinematical information with the microwave spectral data, since they are related in the theories of the positive spectral index that appeared in 1975. The Fabry-Perot observations are reported in Astrophys. J. 1977 September 15. No other journal article is yet in press.

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