The dramatic kinematics of the hydrogen deficient Planetary Nebula Abell 30

1997 ◽  
Vol 180 ◽  
pp. 261-261
Author(s):  
J. Meaburn ◽  
J. A. López
Keyword(s):  
Planetary Nebula ◽  
Velocity Structure ◽  
Spatially Resolved ◽  
San Pedro ◽  
First Time ◽  
Echelle Spectrometer

The remarkable velocity structure of the different components of the hydrogen deficient planetary nebula Abell 30 have been revealed for the first time by obtaining spatially resolved profiles of the [O III] 5007 å lines with the Manchester echelle spectrometer combined with the 2.1 m San Pedro Mártir telescope.

scholarly journals The kinematics of the extensive bipolar lobes and symmetric knots of the Planetary Nebula KjPn 8 (PK 112-001)

1997 ◽  
Vol 180 ◽  
pp. 255-255
Author(s):  
J. A. López ◽  
J. Meaburn ◽  
M. Bryce ◽  
L. F. Rodríguez
Keyword(s):  
Planetary Nebula ◽  
Spatially Resolved ◽  
San Pedro ◽  
Angular Extent ◽  
Echelle Spectrometer

Spatially resolved profiles of the Hα, and [NII] lines have been obtained with the Manchester echelle spectrometer combined with the 2.1 m San Pedro Mártir telescope over the bipolar lobes, the symmetric low ionization knots and the bright core of the planetary nebula KjPn 8. The lobes of this galactic bipolar nebula have the largest angular extent, 14′ × 4′, yet discovered.

scholarly journals Characterization of the planetary nebula Tc 1 based on VLT X-shooter observations

2019 ◽  
Vol 490 (2) ◽  
pp. 2475-2494 ◽  
Author(s):  
Isabel Aleman ◽  
Marcelo L Leal-Ferreira ◽  
Jan Cami ◽  
Stavros Akras ◽  
Bram Ochsendorf ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Three Dimensional ◽  
Central Star ◽  
Gas Temperature ◽  
Spatially Resolved ◽  
Morphological Model ◽  
Density Enhancement ◽  
First Time ◽  
The Empirical Analysis

ABSTRACT We present a detailed analysis of deep VLT/X-Shooter observations of the planetary nebula Tc 1. We calculate gas temperature, density, extinction, and abundances for several species from the empirical analysis of the total line fluxes. In addition, a spatially resolved analysis of the most intense lines provides the distribution of such quantities across the nebula. The new data reveal that several lines exhibit a double peak spectral profile consistent with the blue and redshifted components of an expanding spherical shell. The study of such components allowed us to construct for the first time a three-dimensional morphological model, which reveals that Tc 1 is a slightly elongated spheroid with an equatorial density enhancement seen almost pole on. A few bright lines present extended wings (with velocities up to a few hundred km s−1), but the mechanism producing them is not clear. We constructed photoionization models for the main shell of Tc 1. The models predict the central star temperature and luminosity, as well as the nebular density and abundances similar to previous studies. Our models indicate that Tc 1 is located at a distance of approximately 2 kpc. We report the first detection of the [Kr iii] 6825 Å emission line, from which we determine the Krypton abundance. Our model indicates that the main shell of Tc 1 is matter bounded; leaking H ionizing photons may explain the ionization of its faint AGB-remnant halo.

scholarly journals A detailed spatiokinematic model of the multipolar planetary nebula NGC 7026

2011 ◽  
Vol 7 (S283) ◽  
pp. 332-333 ◽  
Author(s):  
David M. Clark ◽  
Jose Alberto López ◽  
Wolfgang Steffen ◽  
Michael G. Richer
Keyword(s):  
High Resolution ◽  
Planetary Nebula ◽  
Baja California ◽  
Kinematic Model ◽  
X Ray ◽  
3 Dimensional ◽  
San Pedro ◽  
Echelle Spectrometer

AbstractWe present the most extensive, long-slit, high-resolution coverage of the complex planetary nebula (PN), NGC 7026. Ten spectra were acquired 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. Knowledge of the 3-D structure of this nebula is relevant to understand the physics behind the extended X-ray emission in this object.

scholarly journals First record of the sipunculan worm Phascolion (Phascolion) caupo Hendrix, 1975 in the Mediterranean Sea

2012 ◽  
Vol 13 (1) ◽  
pp. 89 ◽  
Author(s):  
L.M. FERRERO-VICENTE ◽  
A. LOYA-FERNANDEZ ◽  
C. MARCO-MENDEZ ◽  
E. MARTINEZ-GARCIA ◽  
J.I. SAIZ-SALINAS ◽  
...  
Keyword(s):  
Mediterranean Sea ◽  
First Record ◽  
Western Mediterranean ◽  
High Load ◽  
San Pedro ◽  
Soft Bottoms ◽  
The Mediterranean ◽  
First Time

Specimens of the sipunculan worm Phascolion (Phascolion) caupo Hendrix, 1975 have been collected for the first time in the Mediterranean Sea, thus increasing the number of known sipunculan species of up to 36 in this area. They were encountered on soft bottoms from the coast of San Pedro del Pinatar (Western Mediterranean). Thirty specimens were collected at a depth ranging from 32.6 to 37.2 m, mainly in sandy substrata with high load of silt and clays. 80% of the individuals were found inhabiting empty shells of gastropods or empty tubes of serpulid polychaetes.

3D ionization structure and kinematics of NGC 2392

2011 ◽  
Vol 7 (S283) ◽  
pp. 348-349
Author(s):  
Reginald J. Dufour ◽  
Jonathan N. Sick ◽  
Patrick M. Hartigan ◽  
Richard B. C. Henry ◽  
Karen B. Kwitter ◽  
...  
Keyword(s):  
Spatial Resolution ◽  
Velocity Structure ◽  
High Spatial Resolution ◽  
Emission Lines ◽  
3 Dimensional ◽  
3D Morphology ◽  
Ionization Structure ◽  
First Time ◽  
Echelle Spectroscopy

AbstractWe discuss the 3D morphology, ionization structure, and kinematics of NGC 2392, the “Eskimo,” based on new and archival HST imagery and new long-slit echelle spectroscopy. High spatial resolution ionization maps of the nebula were made from HST WFPC2 imagery and compared with their velocity structure in various emission lines from echelle spectra taken with the 4m telescope at Kitt Peak. The imagery and spectra were then compared to map the kinematics of the nebula in several emission lines and decode the 3-dimensional morphology and ionization structure of the nebula, including that of C+2 from C III] 1909 Å for the first time.

scholarly journals Mapping the physical and chemical properties of the planetary nebula NGC 3242

2011 ◽  
Vol 7 (S283) ◽  
pp. 448-449
Author(s):  
Hektor Monteiro ◽  
Denise Gonçalves ◽  
Marcelo Leal-Ferreira ◽  
Romano Corradi ◽  
Sebastian Sánchez
Keyword(s):  
Planetary Nebula ◽  
Three Dimensional ◽  
Chemical Properties ◽  
Small Scale ◽  
Chemical Abundances ◽  
Electronic Density ◽  
Spatially Resolved ◽  
Integral Field Spectroscopy ◽  
Main Components ◽  
Physical And Chemical

AbstractWe present optical integral field spectroscopy analysis of the main components, with the exception of the halo, as well as of the detected small-scale structures of the planetary nebulae NGC 3242. The observations were obtained with the VIMOS instrument attached to VLT-UT3. Spatially resolved maps of the electronic density (Ne), temperatures (Te) and chemical abundances, i.e., in a pixel to pixel fashion of the small and large-scales structures of this planetary nebula are determined in this work. These diagnostic and abundance maps represent important constraints for future detailed three dimensional photoionization modeling of the nebula, as well as providing important information on biases introduced by traditional slit observations.

Presence of Dosidicus gigas paralarvae (Cephalopoda: Ommastrephidae) in the central Gulf of California, Mexico related to oceanographic conditions

2010 ◽  
Vol 91 (4) ◽  
pp. 807-814 ◽  
Author(s):  
Susana Camarillo-Coop ◽  
César A. Salinas-Zavala ◽  
Marlenne Manzano-Sarabia ◽  
Eugenio Alberto Aragón-Noriega
Keyword(s):  
Gulf Of California ◽  
Mantle Length ◽  
Dosidicus Gigas ◽  
Potential Fecundity ◽  
San Pedro ◽  
Jumbo Squid ◽  
Ecological Importance ◽  
Santa Rosalia ◽  
First Time ◽  
The Relationship

The jumbo squid Dosidicus gigas is the only ommastrephid commercially caught in Mexico. Despite the economic and ecological importance of this species, little is known about its early life stages. The relationship between the presence of paralarvae and mesoscale oceanic features was investigated for the first time in the central Gulf of California, Mexico in February, April, June and September of 2008. A total of 86 paralarvae were found only in June and September (summer season), in the well-stratified column water where the thermocline was evident and warm sea surface waters (27.7° to 29.4°C) dominated. The greatest abundance of D. gigas paralarvae was observed within 2.23 to 3.48 km of the main front. The mantle length of the smallest paralarvae corresponded with the mantle length at hatching. The San Pedro Mártir Island–Santa Rosalia transect and Santa Rosalia–Guaymas transect were determined as the main hatching localities in June and September respectively. The number of paralarvae found in this study contrast with the potential fecundity of mature females which are found throughout the year.

scholarly journals The Structure and Velocity Field of A78

1989 ◽  
Vol 131 ◽  
pp. 185-185
Author(s):  
P. Pismis ◽  
M. A. Moreno
Keyword(s):  
Velocity Field ◽  
Planetary Nebula ◽  
Image Intensifier ◽  
Radial Velocities ◽  
Central Hole ◽  
Expansion Velocity ◽  
San Pedro ◽  
Systemic Velocity ◽  
Fabry Perot ◽  
The Face

We present a velocity field of the planetary nebula A78 based on three Fabry Pérot Hα (10A) interferograms taken with a focal reducer attached to the 2.1 m reflector of the Observatorio Astronómico Nacional at San Pedro Mártir, Mexico. We have used a single-stage Varo image intensifier and two different étalons with interorder separations of 283 km s−1 (2 interf.) and 100 km s−1 (1 interf.). The scale of the original photographs is 49 arcsec mm−1. Our data have yielded radial velocities in the Hα line at 110 points on the face of A78; the velocity field is far from being smooth. The rings are wide around the central hole, and a few show definite splittings; from these splittings we have estimated an overall expansion velocity of 27 km s−1. The average systemic velocity is found to be around −3 km s−1.

scholarly journals Towards mapping turbulence in the intra-cluster medium

2019 ◽  
Vol 629 ◽  
pp. A143 ◽  
Author(s):  
Nicolas Clerc ◽  
Edoardo Cucchetti ◽  
Etienne Pointecouteau ◽  
Philippe Peille
Keyword(s):  
Monte Carlo ◽  
Structure Function ◽  
Velocity Structure ◽  
High Energy ◽  
Sample Variance ◽  
Physical Parameters ◽  
Sample Mean ◽  
X Ray ◽  
Spatially Resolved ◽  
Mean And Variance

Context. X-ray observations of galaxy clusters provide insights into the nature of gaseous turbulent motions, their physical scales, and the fundamental processes to which they are related. Spatially-resolved, high-resolution spectral measurements of X-ray emission lines provide diagnostics on the nature of turbulent motions in emitting atmospheres. Since they are acting on scales comparable to the size of the objects, the uncertainty on these physical parameters is limited by the number of observational measurements, through sample variance. Aims. We propose a different and complementary approach to repeating numerical simulations for the computation of sample variance (i.e. Monte-Carlo sampling) by introducing new analytical developments for lines diagnosis. Methods. We considered the model of a “turbulent gas cloud”, consisting in isotropic and uniform turbulence described by a universal Kolmogorov power-spectrum with random amplitudes and phases in an optically thin medium. Following a simple prescription for the four-term correlation of Fourier coefficients, we derived generic expressions for the sample mean and variance of line centroid shift, line broadening, and projected velocity structure function. We performed a numerical validation based on Monte-Carlo simulations for two popular models of gas emissivity based on the β-model. Results. Generic expressions for the sample variance of line centroid shifts and broadening in arbitrary apertures are derived and match the simulations within their range of applicability. Generic expressions for the mean and variance of the structure function are provided and verified against simulations. An application to the Athena/X-IFU (Advanced Telescope for High-ENergy Astrophysics/X-ray Integral Field Unit) and XRISM/Resolve (X-ray Imaging and Spectroscopy Mission) instruments forecasts the potential of sensitive, spatially-resolved spectroscopy to probe the inertial range of turbulent velocity cascades in a Coma-like galaxy cluster. Conclusions. The formulas provided are of generic relevance and can be implemented in forecasts for upcoming or current X-ray instrumentation and observing programmes.

Near IR and visual polarimetry of the Planetary Nebula M2-9

2018 ◽  
Vol 14 (S343) ◽  
pp. 480-482
Author(s):  
Silvana G. Navarro ◽  
Omar Serrano ◽  
Abraham Luna ◽  
Rangaswami Devaraj ◽  
Luis J. Corral ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Accretion Disk ◽  
Linear Polarization ◽  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Circumstellar Disk ◽  
Preferential Direction ◽  
Visual Region ◽  
Near Ir ◽  
San Pedro

AbstractBipolar and more complex morphologies observed in planetary nebulae have been explained by two principal hypotheses: by the existence of a companion producing a circumstellar disk, by the effects of a magnetic field, or by a combination of both. The polarimetric analysis of these objects could give information about the presence of dust grains aligned with any preferential direction, due to a magnetic field or to the action of radiative torques (RAT). We performed polarimetric observations of some planetary nebulae in order to detect linear polarization and (in the best scenario) to detect the signature of an accretion disk in these objects. We observed in the visual region with POLIMA at the San Pedro Mártir observatory, and with POLICAN the NIR polarimeter in the Guillermo Haro observatory. We present the result of these observations in one of these objects: the PN M2-9.

Sign in / Sign up

Export Citation Format

Share Document