The SPM kinematic catalogue of Galactic planetary nebulae

López, J. M.; Richer, M. G.; García-Díaz, Ma. T.; Clark, David M.; Meaburn, J.; Riesgo, H.; Steffen, W.; Lloyd, M.

doi:10.1017/s1743921312010708

Cited by 14 publications

(25 citation statements)

References 16 publications

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“…Most of these morphokinematic studies have been performed on relatively large, spatially resolved PNe (e.g. García‐Díaz et al ; Clark et al ; López et al ) but they can also be very revealing when studying spatially unresolved, compact PNe, as we show here.…”

Section: Introductionsupporting

confidence: 51%

“…In this work, we carried out a morphokinematic study of five compact PNe. The data were drawn from the kinematic catalogue of galactic planetary nebulae (López et al ). The sample was selected on the basis of compact PNe with no discernible or apparent structure from their ground‐based images, no high spatial resolution imaging available (e.g.…”

Section: Discussionmentioning

confidence: 99%

“…All spectra were also calibrated to heliocentric velocity. These spectra are part of the kinematic catalogue of galactic planetary (López et al ) and are available at http://kincatpn.astrosen.unam.mx, where images from the digitized sky survey are also shown with the location of the slits overlaid for each object.…”

Section: Observationsmentioning

confidence: 99%

“…No high spatial resolution images for these objects were found in the literature or the usual repositories of images of PNe. These objects were chosen from the San Pedro Mártir kinematic catalogue of galactic planetary nebulae (López et al ) on the basis of their line emission spectra that show the presence of fast, collimated bipolar outflows. The objects selected are M1‐32, M2‐20, M2‐31, M2‐42 and M3‐15.…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional modelling of the collimated bipolar outflows of compact planetary nebulae with Wolf-Rayet-type central stars

Akras

López

2012

Monthly Notices of the Royal Astronomical Society

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We present high-resolution, long-slit spectroscopic observations of five compact (≤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 Mártir kinematic catalogue of galactic planetary nebulae. The central star in four of these objects (M1-32, M2-20, M2-31 and M3-15) is of Wolf-Rayet (WR) type and the fifth object (M2-42) has a weak emission-line star (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 morphokinematic characteristics and reproduce the three-dimensional 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 65-200 km s −1 , whereas the torus/ring component shows much slower expansion velocities, in the range 15-25 km 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 morphokinematic characteristics with the WR-type nuclei deserves further investigation.

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Section: Introductionsupporting

confidence: 51%

Section: Discussionmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Three-dimensional modelling of the collimated bipolar outflows of compact planetary nebulae with Wolf-Rayet-type central stars

Akras

López

2012

Monthly Notices of the Royal Astronomical Society

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“…The spectroscopic observation data used were obtained from the San Pedro Mártir Kinematic Catalog of PNe [8] by directly requesting the spectra of the required object via the email address…”

Section: Spectroscopymentioning

confidence: 99%

Morpho-kinematics study of planetary nebula Sh 2-71 based on astrophysical 3-d modeling

Fajrin

Malasan

Akbar

2022

J. Phys.: Conf. Ser.

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A planetary nebula is formed when a low to intermediate mass star approaches the end of its life. Before the ejected materials finally interact with and dissipate into the interstellar matters, the nebula will be visible surrounding its former stellar core. The variety of planetary nebulae visual appearances indicates that the material ejected and leave the central star behind in unique ways. Morpho-kinematics study aims to find out the 3-d shape using the help of imaging and spectroscopic observations. Imaging allows on to observe the projection of planetary nebulae onto the plane perpendicular to the line of sight to the observer, while spectroscopy gives the ability to infer the expansion characteristics from the spectrum produced by shells within planetary nebulae. We report the 3-d shape modeling of Sh 2-71 (PNG 035.9-01.1, α(J2000.0) = 19h01m59.96s, δ(J2000.0) = 02°09’16.1”) using images obtained from Gemini Multi-Object Spectrograph (GMOS), Hong Kong/Australian Astronomical Observatory/Strasbourg Observatory Ha Planetary Nebula (HASH PN Database), and DSS image combined with high-resolution long-slit spectra from San Pedro Martir Kinematic Catalogue of Planetary Nebulae. The 3-d modeling is carried out with software that specializes in modeling three dimensional astrophysical object SHAPE. The acquired data from observations show that Sh 2-71 possesses a torus with three bipolar lobes while modeling by SHAPE tells that the torus is inclined by 37° and the bipolar lobes are on the same plane.

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Deep high spectral resolution spectroscopy and chemical composition of ionized nebulae

et al. 2014

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High spectral resolution spectroscopy has proved to be very useful for the advancement of chemical abundances studies in photoionized nebulae, such as H II regions and planetary nebulae (PNe). Classical analyses make use of the intensity of bright collisionally excited lines (CELs), which have a strong dependence on the electron temperature and density. By using high resolution spectrophotometric data, our group has led the determination of chemical abundances of some heavy element ions, mainly O ++ , O + and C ++ from faint recombination lines (RLs), allowing us to deblend them from other nearby emission lines or sky features. The importance of these lines is that their emissivity depends weakly on the temperature and density structure of the gas. The unresolved issue in this field is that recombination lines of heavy element ions give abundances that are about 2-3 times higher than those derived from CELs −in H II regions− for the same ion, and can even be a factor of 70 times higher in some PNe. This uncertainty puts into doubt the validity of face values of metallicity that we use as representative not only for ionized nebulae in the Local Universe, but also for star-forming dwarf and spiral galaxies at different redshifts. Additionally, high-resolution data can allow us to detect and deblend faint lines of neutron capture element ions in PNe. This information would introduce further restrictions to evolution models of AGBs and would help to quantify the chemical enrichment in s-elements produced by low and intermediate mass stars. The availability of an echelle spectrograph at the E-ELT will be of paramount interest to: (a) extend the studies of heavyelement recombination lines to low metallicity objects, (b) to extend abundance determinations of s-elements to planetary nebulae in the extragalactic domain and to bright Galactic and extragalactic H II regions. . However, high spectral resolution spectroscopy permits to obtain proper measurements of very faint lines of much interest for abundance studies due to their closeness to other lines or telluric emission features, specially in the reddest part of the op-⋆ Corresponding author. e-mail: cel@iac.es tical range or the near infrared (NIR). In most PNe, high spectral resolution is necessary in order to resolve their usually complex velocity structure, where velocity splitting of the order of few to several tens of km s −1 is the common rule. Since the velocity structure of H II regions is normally much simpler, spectral resolutions of about R∼10,000 are necessary to resolve their line widths and thus optimize the contrast of the faint lines with respect to the underlying continuum. The continuum may be very intense in the case of the spectra of extragalactic H II regions, where most of the contribution comes from the stellar underlying population we are including in our observing area and may even contain absorption features. Moreover, there are also important bright collisionally excited emission lines that need the use of high spectral resolution −R∼3000 ...

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The SPM kinematic catalogue of Galactic planetary nebulae

Cited by 14 publications

References 16 publications

Three-dimensional modelling of the collimated bipolar outflows of compact planetary nebulae with Wolf-Rayet-type central stars

Three-dimensional modelling of the collimated bipolar outflows of compact planetary nebulae with Wolf-Rayet-type central stars

Morpho-kinematics study of planetary nebula Sh 2-71 based on astrophysical 3-d modeling

Deep high spectral resolution spectroscopy and chemical composition of ionized nebulae

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