-
[show abstract]
[hide abstract]
ABSTRACT: The 3-D and kinematic structure of the Eskimo nebula, NGC 2392, has been
notoriously difficult to interpret in detail given its complex morphology,
multiple kinematic components and its nearly pole-on orientation along the line
of sight. We present a comprehensive, spatially resolved, high resolution,
long-slit spectroscopic mapping of the Eskimo planetary nebula. The data
consist of 21 spatially resolved, long-slit echelle spectra tightly spaced over
the Eskimo and along its bipolar jets. This data set allows us to construct a
velocity-resolved [NII] channel map of the nebula with a resolution of 10 km/s
that disentangles the different kinematic components of the nebula. The
spectroscopic information is combined with HST images to construct a detailed
three dimensional morpho-kinematic model of the Eskimo using the code SHAPE.
With this model we demonstrate that the Eskimo is a close analog to the Saturn
and the Cat's Eye nebulae, but rotated 90 degrees to the line of sight.
Furthermore, we show that the main characteristics of our model apply to the
general properties of the group of elliptical planetary nebulae with ansae or
FLIERS, once the orientation is considered. We conclude that these kind of
nebulae belongs to a class with a complex common evolutionary sequence of
events.
11/2012;
-
[show abstract]
[hide abstract]
ABSTRACT: We present an extensive, long-slit, high-resolution coverage of the complex
planetary nebula (PN), NGC 7026. We acquired ten spectra using the Manchester
Echelle Spectrometer at San Pedro Martir Observatory in Baja California,
Mexico, and each shows exquisite detail, revealing the intricate structure of
this object. Incorporating these spectra into the 3-dimensional visualization
and kinematic program, SHAPE, and using HST images of NGC 7026, we have
produced a detailed structural and kinematic model of this PN. NGC 7026
exhibits remarkable symmetry consisting of three lobe-pairs and four sets of
knots, all symmetrical about the nucleus and displaying a conical outflow.
Comparing the 3-D structure of this nebula to recent, XMM-Newton X-ray
observations, we investigate the extended X-ray emission in relation to the
nebular structure. We find that the X-ray emission, while confined to the
closed, northern lobes of this PN, shows an abrupt termination in the middle of
the SE lobe, which our long slit data shows to be open. This is where the
shocked, fast wind seems to be escaping the interior of the nebula and the
X-ray emission rapidly cools in this region.
10/2012;
-
[show abstract]
[hide abstract]
ABSTRACT: We present high-resolution, long-slit spectroscopic observations of five
compact ($\leq$ 10 arcsec) planetary nebulae located close to the galactic
bulge region and for which no high spatial resolution images are available. The
data have been drawn from the San Pedro M\'artir kinematic catalogue of
galactic planetary nebulae (L\'opez et al. 2012). The central star in four of
these objects (M 1-32, M 2-20, M 2-31 and M 3-15) is of WR-type and the fifth
object (M 2-42) has a wels type nucleus. These observations reveal the presence
in all of them of a dense and thick equatorial torus-like component and
high-speed, collimated, bipolar outflows. The code SHAPE is used to investigate
the main morpho-kinematic characteristics and reproduce the 3-D structure of
these objects assuming a cylindrical velocity field for the bipolar outflows
and a homologous expansion law for the torus/ring component. The deprojected
expansion velocities of the bipolar outflows are found to be in the range of 65
to 200 km $\rm{s^{-1}}$, whereas the torus/ring component shows much slower
expansion velocities, in the range of 15 to 25 km $\rm{s^{-1}}$. It is found
that these planetary nebulae have very similar structural components and the
differences in their emission line spectra derive mostly from their different
projections on the sky. The relation of their morpho-kinematic characteristics
with the WR-type nuclei deserves further investigation.
06/2012;
-
[show abstract]
[hide abstract]
ABSTRACT: The kinematics of the bipolar planetary nebulae Hb~5 and K 3-17 are
investigated in detail by means of a comprehensive set of spatially resolved
high spectral resolution, long-slit spectra. Both objects share particularly
interesting characteristics, such as a complex filamentary, rosette-type
nucleus, axial point-symmetry and very fast bipolar outflows. The kinematic
information of Hb~5 is combined with {\it HST} imagery to construct a detailed
3D model of the nebula using the code SHAPE. The model shows that the large
scale lobes are growing in a non-homologous way. The filamentary loops in the
core are proven to actually be secondary lobes emerging from what appears to be
a randomly punctured, dense, gaseous core and the material that forms the point
symmetric structure flows within the lobes with a distinct kinematic pattern
and its interaction with the lobes has had a shaping effect on them. Hb~5 and
K~3-17 may represent a class of fast evolving planetary nebulae that will
develop poly-polar characteristics once the nebular core evolves and expands.
03/2012;
-
[show abstract]
[hide abstract]
ABSTRACT: We present a set of optical and infrared images combined with long-slit,
medium and high dispersion spectra of the southern planetary nebula (PN) NGC
5189. The complex morphology of this PN is puzzling and has not been studied in
detail so far. Our investigation reveals the presence of a new dense and cold
infrared torus (alongside the optical one) which probably generated one of the
two optically seen bipolar outflows and which might be responsible for the
twisted appearance of the optical torus via an interaction process. The
high-resolution MES-AAT spectra clearly show the presence of filamentary and
knotty structures as well as three expanding bubbles. Our findings therefore
suggest that NGC 5189 is a quadrupolar nebula with multiple sets of symmetrical
condensations in which the interaction of outflows has determined the complex
morphology.
03/2012;
-
[show abstract]
[hide abstract]
ABSTRACT: The San Pedro M\'artir kinematic catalogue of galactic planetary nebulae
provides spatially resolved, long-slit Echelle spectra for about 600 planetary
nebulae. The data are presented wavelength calibrated and corrected for
heliocentric motion. For most objects multiple spectra have been acquired and
images with accurate slit positions on the nebulae are also presented for each
object. This is the most extensive and homogeneous single source of data
concerning the internal kinematics of the ionized nebular material in planetary
nebulae. Data can be retrieved for individual objects or selected by groups
that share some common characteristics, such as by morphological classes,
galactic population, binary cores, presence of fast outflows, etc. The
catalogue is available through the world wide web at
http://kincatpn.astrosen.unam.mx .
10/2011;
-
[show abstract]
[hide abstract]
ABSTRACT: We have obtained images and long-slit, spatially resolved echelle spectra for
twenty four planetary nebulae (PNe) that have confirmed close binary nuclei.
The sample shows a variety of morphologies, however toroids or dense equatorial
density enhancements are identified, both in the imagery and the spectra, as
the common structural component. These toroids are thought to be the remnant
fingerprints of the post common envelope phase. Based on the characteristics of
the present sample we suggest a list of additional PNe that are likely to host
close binary nuclei
01/2011;
-
[show abstract]
[hide abstract]
ABSTRACT: NGC 6751 is a highly structured multiple-shell planetary nebula (PN) with a bipolar outflow. In this work, we present a comprehensive set of spatially resolved, high spectral resolution, long-slit spectra and deep imaging from San Pedro Mártir, Gemini, the Hα composite full sky survey and archive images from the Hubble Space Telescope and Spitzer. This material allows us to identify all the main morphological components and study their detailed kinematics. We find a thick equatorial structure fragmented into multiple knots that enclose a fast expanding bubble with a filamentary surface structure. The knotty ring is surrounded by faint emission from a disk-like envelope. Lobes with embedded filaments form a bipolar outflow. The equatorial ring is tilted with respect to the line of sight and with respect to the bipolar outflow. A spherical halo surrounds the PN and there is material further out identified as a fragmented outer halo. This information is used to derive a three-dimensional morpho-kinematic model using the code SHAPE that closely replicates the observed image and long-slit spectra of the nebula, providing a fair representation of its complex structure. NGC 6751 is located close to the galactic plane and its large-scale surrounding environment is shown to be a gas-rich region. We find indications that the PN is interacting with the interstellar medium. Emission components from an extended nebulosity located a couple of arcminutes away from the nebula have radial velocities that are inconsistent with the rest of NGC 6751 and are confirmed as originating from the ambient material, not related to the PN, in agreement with a previous suggestion.
The Astrophysical Journal 09/2010; 722(2):1260. · 6.02 Impact Factor
-
[show abstract]
[hide abstract]
ABSTRACT: We present the first detailed spatio-kinematical analysis and modelling of the planetary nebula Abell~41, which is known to contain the well-studied close-binary system MT Ser. This object represents an important test case in the study of the evolution of planetary nebulae with binary central stars as current evolutionary theories predict that the binary plane should be aligned perpendicular to the symmetry axis of the nebula. Longslit observations of the \NII\ emission from Abell~41 were obtained using the Manchester Echelle Spectrometer on the 2.1-m San Pedro M\'artir Telescope. These spectra, combined with deep, narrowband imagery acquired using ACAM on the William Herschel Telescope, were used to develop a spatio-kinematical model of \NII\ emission from Abell~41. The best fitting model reveals Abell~41 to have a waisted, bipolar structure with an expansion velocity of $\sim$40\kms{} at the waist. The symmetry axis of the model nebula is within 5$^\circ$ of perpendicular to the orbital plane of the central binary system. This provides strong evidence that the close-binary system, MT Ser, has directly affected the shaping of its host nebula, Abell~41. Comment: 4 pages, 2 figures, to appear in the proceedings of the conference "Asymmetric Planetary Nebulae V", eds. Zijlstra, et al., editorial: Ebrary
09/2010;
-
[show abstract]
[hide abstract]
ABSTRACT: We present the first detailed spatio-kinematical analysis and modelling of
the planetary nebula Abell 41, which is known to contain the well-studied
close-binary system MT Ser. This object represents an important test case in
the study of the evolution of planetary nebulae with binary central stars as
current evolutionary theories predict that the binary plane should be aligned
perpendicular to the symmetry axis of the nebula.
Deep narrowband imaging in the light of [NII], [OIII] and [SII], obtained
using ACAM on the William Herschel Telescope, has been used to investigate the
ionisation structure of Abell 41. Longslit observations of the H-alpha and
[NII] emission were obtained using the Manchester Echelle Spectrometer on the
2.1-m San Pedro M\'artir Telescope. These spectra, combined with the narrowband
imagery, were used to develop a spatio-kinematical model of [NII] emission from
Abell 41. The best fitting model reveals Abell 41 to have a waisted, bipolar
structure with an expansion velocity of ~40km\s at the waist. The symmetry axis
of the model nebula is within 5$\degr$ of perpendicular to the orbital plane of
the central binary system. This provides strong evidence that the close-binary
system, MT Ser, has directly affected the shaping of its nebula, Abell 41.
Although the theoretical link between bipolar planetary nebulae and binary
central stars is long established, this nebula is only the second to have this
link, between nebular symmetry axis and binary plane, proved observationally.
06/2010;
-
[show abstract]
[hide abstract]
ABSTRACT: We study the line widths in the [\ion{O}{3}]$\lambda$5007 and H$\alpha$ lines for two groups of planetary nebulae in the Milky Way bulge based upon spectroscopy obtained at the Observatorio Astron\'omico Nacional in the Sierra San Pedro M\'artir (OAN-SPM) using the Manchester Echelle Spectrograph. The first sample includes objects early in their evolution, having high H$\beta$ luminosities, but [\ion{O}{3}]$\lambda 5007/\mathrm H\beta < 3$. The second sample comprises objects late in their evolution, with \ion{He}{2} $\lambda 4686/\mathrm H\beta > 0.5$. These planetary nebulae represent evolutionary phases preceeding and following those of the objects studied by Richer et al. (2008). Our sample of planetary nebulae with weak [\ion{O}{3}]$\lambda$5007 has a line width distribution similar to that of the expansion velocities of the envelopes of AGB stars, and shifted to systematically lower values as compared to the less evolved objects studied by Richer et al. (2008). The sample with strong \ion{He}{2} $\lambda 4686$ has a line width distribution indistinguishable from that of the more evolved objects from Richer et al. (2008), but a distribution in angular size that is systematically larger and so they are clearly more evolved. These data and those of Richer et al. (2008) form a homogeneous sample from a single Galactic population of planetary nebulae, from the earliest evolutionary stages until the cessation of nuclear burning in the central star. They confirm the long-standing predictions of hydrodynamical models of planetary nebulae, where the kinematics of the nebular shell are driven by the evolution of the central star. Comment: accepted for publication in the Astrophysical Journal
04/2010;
-
M. G. Richer, J. A. López,
E. Díaz-Méndez,
H. Riesgo,
S. -H. Báez,
Ma. T. García Díaz,
J. Meaburn,
D. M. Clark,
R. M. Calderón Olvera,
G. López Soto,
O. Toledano Rebolo
[show abstract]
[hide abstract]
ABSTRACT: We present kinematic data for 211 bright planetary nebulae in eleven Local Group galaxies: M31 (137 PNe), M32 (13), M33 (33), Fornax (1), Sagittarius (3), NGC 147 (2), NGC 185 (5), NGC 205 (9), NGC 6822 (5), Leo A (1), and Sextans A (1). The data were acquired at the Observatorio Astron\'omico Nacional in the Sierra de San Pedro M\'artir using the 2.1m telescope and the Manchester Echelle Spectrometer in the light of [\ion{O}{3}]$\lambda$5007 at a resolution of 11 km/s. A few objects were observed in H$\alpha$. The internal kinematics of bright planetary nebulae do not depend strongly upon the metallicity or age of their progenitor stellar populations, though small systematic differences exist. The nebular kinematics and H$\beta$ luminosity require that the nebular shells be accelerated during the early evolution of their central stars. Thus, kinematics provides an additional argument favoring similar stellar progenitors for bright planetary nebulae in all galaxies. Comment: Accepted for publication in the October 2010 issue of the Revista Mexicana de Astronom\'ia y Astrof\'isica
04/2010;
-
M. G. Richer, J. A. López,
E. Díaz-Méndez,
Riesgo H,
Báez S.-H,
Ma. T. García Díaz,
Meaburn J,
D. M. Clark,
R. M. Calderón Olvera,
G. López Soto,
O. Toledano Rebolo
[show abstract]
[hide abstract]
ABSTRACT: Presentamos datos cinemáticos para 211 nebulosas planetarias brillantes en once galaxias del Grupo Local: M31 (137 NPs), M32 (13), M33 (33), Fornax (1),Sagittarius (3), NGC 147 (2), NGC 185 (5), NGC 205 (9), NGC 6822 (6), Leo A (1), y Sextans A (1). Adquirimos los datos en el Observatorio Astronómico Nacional en la Sierra de San Pedro Mártir con el telescopio de 2.1 m y el espectrómetro Manchester Echelle en la línea de [O III]l 5007 con una resolución de 11 km s¿1. Observamos algunos objetos en H¿. La cinemática de nebulosas planetarias brillantes no depende fuertemente de la metalicidad o la edad de la población estelar progenitora en sus galaxias huéspedes, aunque existen pequeñas diferencias sistemáticas. La cinemática y la luminosidad en Hb de las cáscaras nebulares requieren la aceleraci ón de las cáscaras durante la evolución temprana de las estrellas centrales. Así, la cinemática representa otro argumento a favor de estrellas progenitoras similares para las nebulosas planetarias brillantes en todas galaxias.
Revista Mexicana de Astronomía y Astrofísica : Universidad Nacional Autónoma de México. Instituto de Astronomía. 01/2010;
-
[show abstract]
[hide abstract]
ABSTRACT: We present a detailed kinematical analysis of the young compact hourglass-shaped planetary nebula Hb 12. We performed optical imaging and longslit spectroscopy of Hb 12 using the Manchester echelle spectrometer with the 2.1m San Pedro Martir telescope. We reveal, for the first time, the presence of end caps (or knots) aligned with the bipolar lobes of the planetary nebula shell in a deep [NII]6584 image of Hb 12. We measured from our spectroscopy radial velocities of 120 km/s for these knots. We have derived the inclination angle of the hourglass shaped nebular shell to be 65 degrees to the line of sight. It has been suggested that Hb 12's central star system is an eclipsing binary (Hsia et al. 2006) which would imply a binary inclination of at least 80 degrees. However, if the central binary has been the major shaping influence on the nebula then both nebula and binary would be expected to share a common inclination angle. Finally, we report the discovery of high-velocity knots with Hubble-type velocities, close to the core of Hb 12, observed in Halpha and oriented in the same direction as the end caps. Very different velocities and kinematical ages were calculated for the outer and inner knots showing that they may originate from different outburst events. Comment: 9 pages, 6 figures, accepted for publication in MNRAS
05/2009;
-
[show abstract]
[hide abstract]
ABSTRACT: NGC 6337 is a member of the rare group of planetary nebulae where a close
binary nucleus has been identified. The nebula's morphology and emission line
profiles are both unusual, particularly the latter. We present a thorough
mapping of spatially resolved, long-slit echelle spectra obtained over the
nebula that allows a detailed characterization of its complex kinematics. This
information, together with narrow band imagery is used to produce a three
dimensional model of the nebula using the code SHAPE. The 3-D model yields a
slowly expanding toroid with large density fluctuations in its periphery that
are observed as cometary knots. A system of bipolar expanding caps of low
ionization are located outside the toroid. In addition, an extended high
velocity and tenuous bipolar collimated outflow is found emerging from the core
and sharply bending in opposite directions, a behavior that cannot be accounted
for by pure magnetic launching and collimation unless the source of the outflow
is precessing or rotating, as could be expected from a close binary nucleus.
05/2009;
-
[show abstract]
[hide abstract]
ABSTRACT: High spectral resolution observations of the [N II] 6548 + 6584 Å and Hα emission lines from the young planetary nebula MyCn 18 have been obtained using the Manchester echelle spectrometer combined with the Anglo-Australian Telescope. These spatially resolved spectra reveal not only the kinematical characteristics of the two bright rings of emission, which define the well-known "engraved hourglass" structure of this object, but also the dramatic motions of the faint, irregular knots of emission observed outside the main nebular structure. The knots are moving with velocities ≥500 km s-1 away from the central star, an order of magnitude faster than the motions observed from the main nebula, making them among the highest velocity outflows ever observed from a planetary nebula. A bipolar, rotating, episodic jet mechanism is favored for their origin.
The Astrophysical Journal 01/2009; 487(2):L161. · 6.02 Impact Factor
-
[show abstract]
[hide abstract]
ABSTRACT: A disk of excited H2v=1 → 0 S(1) (2.122 μm) emission has been found in the core of the extraordinary bipolar planetary nebula KjPn 8. This surrounds the central, extended, and clumpy thermal radio emission (VLA) and near-infrared (J, H, and K' bands) source. The H2 disk is found to be contained within a previously found expanding CO disk, and they share the same orientation. The plane of the H2 disk is perpendicular to the high-velocity bipolar outflows. The 4'' diameter core of KjPn 8 has also been observed for 37 on-source hours at a wavelength of 6 cm with the MERLIN radio interferometer with an angular resolution of 005. The data have been combined with 4 hr of VLA-A observations at the same wavelength but where the resolution is 05. The most remarkable feature of these radio observations is the possible presence of a weak "point" radio source embedded in the center of the H2 disk. It is thought plausible that this point source may be direct emission from the powerful, ionized wind of the central star that now drives this nebulosity.
The Astrophysical Journal 01/2009; 518(2):778. · 6.02 Impact Factor
-
Asymmetrical Planetary Nebulae IVAsymmetrical Planetary Nebulae IV; 01/2009
-
[show abstract]
[hide abstract]
ABSTRACT: We present high resolution spectroscopy in the [O III]-5007 and Hf lines of bright planetary nebulae in the Milky Way bulge and the dwarf galaxies M32, Fornax, Sagittarius, and NGC 6822 obtained at the Observatorio Astronómico Nacional in the Sierra San Pedro Mártir using the Manchester Echelle Spectrograph. We use the high signal-to-noise (S/N) observations of Milky Way bulge planetary nebulae to explore what kinematic information can be determined reliably when observing extragalactic planetary nebulae in the [O III]-5007 line at modest S/N.We find that the intrinsic line widths measured in [O III]-5007 and Hf are very similar. Over the range of S/N available in this sample, the line width we measure is independent of the S/N. Finally, deviations from a Gaussian line shape are small. Thus, the line width of the [O III]-5007 line in bright extragalactic planetary nebulae should re ect the kinematics of most of the mass in the ionized nebular shell.
Revista Mexicana de Astronomía y Astrofísica : Universidad Nacional Autónoma de México. Instituto de Astronomía. 01/2009;
-
[show abstract]
[hide abstract]
ABSTRACT: Spatially resolved profiles of the Hα and [N II] λ6584 emission lines have been obtained, with the Manchester Echelle Spectrometer on the San Pedro Martir telescope, across the 7'-long nebulous lobe projecting to the east of P Cygni. The kinematics of this giant lobe indicate convincingly that it is a consequence of a highly asymmetric ejection from this volatile star. There is some evidence that the lobe is the northern wall of a hollow, outflowing cavity, but this suggestion needs to be investigated further. A more intriguing possibility is that it is the manifestation of an outflowing "funnel" of gas from P Cygni.
The Astrophysical Journal 12/2008; 516(1):L29. · 6.02 Impact Factor
