Akito Tajitsu

HaTr 10, a Planetary Nebula with Extremely Strong Nitrogen Lines

ABSTRACT Optical spectra and direct images reveal that a very faint, scarcely studied object (HaTr 10) which appears as an incomplete elliptical ring of 0 \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape

Analysis of Internal Motions in the Halo Planetary Nebula H4-1

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G247.8+4.9: A Newly Discovered Optical Supernova Remnant in Puppis

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Expansion Analyses on Planetary Nebulae

ABSTRACT Up to now, 10 planetary nebulae have been regarded as halo planetary nebulae (halo PNe). We obtained low‐ and moderate‐dispersion spectra of the spatially resolved halo planetary nebula H4‐1 in the wavelength region of 3700–6800 A with the Cassegrain Spectrograph of the 74 inch telescope. At moderate dispersions, we were able to observe [O iii] λλ4959, 5007 and Hα of H4‐1 at several position angles (P.A.). We assumed that the widths of these emission‐line profiles were due to Doppler broadening and that these emission lines were composed of several Gaussian components. Multiple Gaussian deconvolution analysis of such emission lines indicated H4‐1 has broad wing components (∼600 km s−1) at P.A. 135° and 180°. We think H4‐1 has a “bipolar flow” between P.A. 135° and 180°. From low‐dispersion spectra, we confirm that H4‐1 is a metal‐poor PN. In spite of the lack of spatially resolved images at present, we believe that H4‐1 has a bipolar flow and that its axis is almost parallel to the line of sight,...

High Velocity Collimated Flow in a Halo Planetary Nebula, H 4-1

As a first step to investigate a newly detected possible supernova remnant in Puppis, a few optical spectra have been obtained. The spectra of this extremely faint nebula, although of poor quality, show strong (N ii) 6583/6548 A u emission. Radial velocities derived from the (N ii) 6583 A u line amount to 50 km s 1 , for both the easternmost and westernmost optical borders of the nebula, and a distinctly blueshifted velocity relative to this value for an emission region close to the eastern rim. In order to check whether the remnant might be akin to the nebula W50 associated with the compact source SS 433, a spectrum of four stars near the center of the image of the nebula was taken; it showed them to be of quite ordinary type and exhibits some traces of (nebular) (N ii) 6583 A u emission. No IRAS source is located at or within the boundaries of the nebula, which coincides with an extended radio source of about 78 mJy at 4850 MHz. The star that gave rise to the remnant may have been a remote member of the Pup OB2 association, at a distance of about 5 kpc.

A New Distance Indicator to Galactic Planetary Nebulae Based upon IRAS Fluxes

Since planetary nebulae(PNe) are defined as the expanding ionized gas surrounding hot central stars, the most important and fundamental subject is to study expansion characteristics. What and how can we determine a typical expansion velocity of individual nebula? In spite of great success of Perek and Kohoutek Catalog(1967) and a recent Strasbourg-ESO Catalogue(992), PNe researchers have suffered from the lack of sufficiently large samples of expansion measurements on various type of PNe.

The Fiber Multi-Object Spectrograph for the Okayama 188cm Telescope - Development and Observation -

H 4-1, PNG 049.3+88.1 (α = 12h59m27.6s, δ = +27°38′14″, 2000), was one of well known halo Planetary Nebulae (PNe). During our program to study the expanding characteristics of PNe, the long-slit spectroscopic observations were made by the cassegrain spectrograph of the 74 inch telescope at the Okay ama Astrophysical Observatory in March 1995.